Iraf-data Reduction Guide Chris

COMMAND OVER COMMANDS

An Astronomers data reduction Guide( IRAF and Linux etc. )

WRITTEN BY

M.CHRISPHIN KARTHICK, ARIES20062007,

Nainital.

Preface This guide is good to start for beginner and expert to recall. The most of the topics andcommands may available from anywhere or from internet, but here it has written only which is mostoften used in data reduction . Also ,the last page attached with all the software’s which is requiredfor data reduction for installation purpose and including some important websites which is necessaryfor an Astronomer. So at the most which is reducing your time to spend on the internet and getting thedetails. For soft copy and important links log on http://aries.ernet.in/page_chrisphin.html. WhileUsing this guide mean time cross check with the expert if any corrections are there. In this guide ifyou have any feedback or queries ,please write to [email protected] [email protected].

Yours M.Chrisphin Karthick,

Known is a DROPUnknown is an OCEAN

Last edited :22 November 2007

Contents

1. Linux commands01

2. Summary of preprocessing08

3. IRAF Commands (Before Basic reduction )09

4. Setting observatory16

5. Setting Air mass 17

6. Basic Reduction18

7. Alignment25

8. Cosmic ray reduction through MIDAS29

9. Cosmic ray reduction through IRAF34

10. Aperture Photometry35

11. Spectroscopy reduction48

Wavelength Calibration52

Flux Calibration 55

Some more hints on spectroscopy reduction59

12. LATEX Introduction64

13. Ellipse Fitting67

14. Iraf Installation78

How it's works—80

Appendix

I. General 91

II. Air mass Calculation Program92

III. FEAR FeAr Line List 3000A10,000A by D. Willmarth93

IV. Spectrum Extinction file for IAO (spec_ext.dat)94

V. Extinction Coefficients for ARIES97

VI. Site Characteristics of HCT 99

VII. Extinction and Sky Brightness for HCT 100

VIII. Halpha filter response curve for HCT 101

IX. FeAr wavelength identification1—102

X. FeAr wavelength identification2 103

XI.FeNe wavelength identification104

XII.Standard calibration data for extinction from IRAF105

Command over commands Chrisphin Karthick,ARIES20062007

1Linux commandsFrom open terminal:>ls To list out >mkdir foldernamemaking a directory>rm f (directory name) removing directory >rm rf (directory name)for removing subdirectories also(* always represents for bulk files or folders)>cp <source> <destination>for copy >cp –r <source> <destination>whole directory>mv <source> <destination>for move>mv <source> <destination>for renaming also>pwdpresent working directory>cd <directoryname>changing directory>cd >coming out to the home.>cd .. >coming out one step back from the source directorygzip filefor making .zip >gunzip filename.gz for unzip >gunzip *.gzfor unzipping lot of files>tar xvpf filename.tar for untar >tar xvf <filename> to extract the tar file>tar zxvf <filename> To extract the tar and zipped file>tar cvf filename.tar filename making tar>zcat <filename.tar.gz> | tar xvf for removing zip and tar in one time the command is > find . name "filename"For finding one file within the computer (or) >lpr P <printerName> <filename> for printing>lpr <filename>if you don’t want mention particular printer by default printer printing>lpqto list out the printing materials: ( it will come as file name and with its number)>lprm <therespectivenumber>to stop the priniting material: >gthump <photo filename>For viewing photo:alt+EscTo switch over to another window; alt+tabTo view and select the alternate window: ctrl+alt+backspace for logout>rebootto reboot the computer.to run latex; >latex <file name>

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>dvips <latexoutputfile> o <newfilename.ps> (OR) >dvips o <.ps> <latexoutputfile.dvi> >gv < .ps>>man commandnamefor help on any commands.> xpdf <file name>to open pdf document:(OR)> gv <file name>> ooffice <filename.ppt>to open ppt:>ps2pdf <filename.ps> <filename.pdf>To change .ps file to .pdf file>du s to check disk space in a directory 13026152 >ps afto display all the processes running on the hostUID PID PPID C STIME TTY TIME CMD501 3618 3545 0 11:00 pts/1 00:00:00 ps af> du kTo report size (in kBytes) of all enclosed directories (recursive)> du ms *To report size (in kBytes) of all enclosed directories (nonrecursive)> usersTo list login IDs of users currently logged in to the system

Transwering data's from one computer to another:>ps –aux | grep <filename>listing out the particular file running on the terminal ID>ftp <that computer number>means >ftp IPaddress OR>gftp username@IPaddress or generally >sftp username@IPaddressthen mget* or mput*or >scp –r username@IPaddress: pathway of file or folder>yum install softwarenamefor installing anything in new fedora version.

For creating webpage

>mozillathen from file GO EDIT PAGE then from edit page file GO COMPOSURE PAGEnow start work .

to get the details of memory capacity of all ....chrisphin > dfFilesystem 1Kblocks Used Available Use% Mounted on

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/dev/sda8 12096724 8125824 3356416 71% //dev/sda6 101086 11153 84714 12% /boot/dev/sda10 18326876 77888 17318024 1% /datanone 253436 0 253436 0% /dev/shm/dev/sda5 10231392 1241840 8989552 13% /dos/dev/sda7 25197220 19620160 4297084 83% /home

working from another computer to our computer then...type..xhost+>ssh X chrisphin @ 202.141.125.144

chrisphin>ls lrt to know the recent downloaded file.total 101456drwxrxrx 2 chrisphin chrisphin 4096 Mar 19 2001 libdrwxrwxrx 3 chrisphin chrisphin 4096 Nov 4 2005 updatednewsdrwxrwxr 7 chrisphin chrisphin 4096 Jul 27 09:52 imagesrwrwr 1 chrisphin chrisphin 1937248 Jul 27 09:52 Firefox_wallpaper.pngdrwxrwxrx 2 chrisphin chrisphin 4096 Jul 27 12:31 uparm

>clearto clear the terminal>setupto set up the configuration of computer.

for .fits file getting details from the terminal...type>more <filename>cosmic > more csa104b02.fitsSIMPLE = T / Fits standardBITPIX = 32 / Bits per pixelNAXIS = 2 / Number of axesNAXIS1 = 1024 / Axis lengthNAXIS2 = 1024 / Axis lengthEXTEND = T / File may contain extensionsORIGIN = 'ESOMIDAS' / FITS file originatorDATE = '20060731T08:43:32' / Date FITS file was generatedIRAFTLM= '10:41:08 (03/08/2006)' / Time of last modificationOBJECT = 'sa104 ' / Name of the object observedCOMMENT NOST 1002.0: Hanisch,R. et al. 2001, Astron. & Astrophys. 376, 559

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CRPIX1 = 1. / Reference pixelCRVAL1 = 1. / Coordinate at reference pixelCDELT1 = 1. / Coord. incr. per pixel (original value)CTYPE1 = ' ' / Units of coordinateCRPIX2 = 1. / Reference pixelCRVAL2 = 1. / Coordinate at reference pixelCDELT2 = 1. / Coord. incr. per pixel (original value)CTYPE2 = ' ' / Units of coordinateBUNIT = ' ' / Units of data valuesDATAMAX = 437.2375 / Maximum data valueRA = 12:42:22 / MIDAS desc.: O_POS(1)DEC = 00:40:00 / MIDAS desc.: O_POS(2)DATEOBS= '20060503T17:01:25' / MIDAS desc.: O_TIME(1)TMSTART= 0. / MIDAS desc.: O_TIME(5)EXPTIME = 260. / MIDAS desc.: O_TIME(7)EPOCH = 2000ST = 13.085UT = 17.02361AIRMASS = 1.146693UTMIDDLE= '17:03:35.0'

Notes:always name the file without space.(if space is ther mv or cp or any command wont work)ex:file name: optical telescope.doc (wrong)file name : opticaltelescope.doc (right)

**If the bookmark has been hidden by sekecting aniother profile to retrive it go to chrisphin>cd .mozilla/.mozilla>ls>cd firefox>lschrisphin default>cd chrisphin>ls>vi bookmark.htmlchrisphin>firefox&

>mplayer <filename.avi>To play the .avi format movie.chrisphin > bc lqFor using terminal as a calculator1+12:quit

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writting a program and executing:>vi <filename>.................:wqSome version problem while transforming tex file (gvim to vi somethinlg like that)in vi file u may come across the problem of ^Mthen :%s/^M/ /g>c++ <filename> (for combiling)>.a/. out

sort all the files w.r.t.to time:>ls lrt

>vol for volume.

Using as super user >su >user name:>password:

while deleting press shift+delete (by right click)...then it wont go to the recycle bin.(in windows)

For making use of alias command:>vi .cshrc

alias x "ds9 &; xgterm.fedora & "alias hedit "/home/chrisphin/bin/./hedit"alias aries "cd /home/chrisphin/data/ariesasper25oct06fits"~~:wq>source .cshrc>rehash .cshrc>now execute the respective it will work.

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example:[chrisphin@aries25 ~]$ aries[chrisphin@aries25 ariesasper25oct06fits]$

To know that which shell we are working :[chrisphin@aries25 ~]$ echo $SHELL/bin/cshfor changing the shell type[chrisphin@aries25 ~]$chshpassword:changing the shell type >cshthen for making alias commands......]vi .cshrc or vi .bashrc depends on the shell........then inside vi editor type

alias x “xgterm&;ds9&;”:wq

To configure the computer IP address:>cd /sbin>ls ifco*> ./ifconfig(Then number and other details will come)

for writing into cd:go to the root >supassword>xcdroast(but before that confirm that whether it is installed xcdroast in /usr/bin)

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Installation of real player in linuxdownload the filethen> chmod a+x <filename.bin> (making executable by changing the mode)

> ./<filename.bin>that,s it.

>xmms&For hearing songs linux the command is

(for installing anything like this ...download RPM file and double click it it will ask for root paswordthat is it it will install automatically.(in fedora core 5 version..that also noneed type yum install<installing file> it will install)

How to write and execute the c programme:1.make a folder within that...within that make one file...programm file ...write by vi editer.that file extensions with .c(for c) or .cpp (for c++)...like file.c or file.cpp>gcc o o_file file.cor >c++ file.cpp

For making alias commands:

chrisphin~>vi .bashrc

PS1="\u\w"\> (this command is for setting the prompt)alias x="xgterm.fedora & ds9&"alias e="emacs &"alias rm="rm i"alias rmr="rmr i"alias g="gomidas"

:wq

chrisphin~>source .bashrc

For bringing scroll bar into iraf the command is as follow and also

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midas wavelength calibration files is as attachment see the attachment below thanks:.....xgterm sb fn 10*20 &

1.1Printer Configuration for ARIES

adding a printer or printer settings:go to system settingprinting

printer name:DN2420networked jet direct202.141.125.4 port:9100HPLASER JET 2420(if not any 2300)finish.

2.Summary of preprocessing:

1. Converting file into fits format.2. Setting Observatory*3. Setting Airmass*4. Making Master biasBias subtraction5. Making Master flat and then Normalized flat for respective filter divide it.

i. e.,{The final image= (raw image – master bias) / normalized flat(how to normalise a flat...take the mean counts of master flat and divide the master flat by that)}

6. Align it.7. Trim it.8. Cosmic rays removal.9. Cleaned image is ready.

(*In the above mentioned steps where 2 and 3 you can do it later also if needed).

Easy way to handling the file and folder name :In this book Prefix given to the file as...object_r1.fits object _filter nth frame.(here example taken as r—filter)bi_1.fitsbias_nth framefl_r1.fitsflat_filter nth framembi.fitsmaster biasmfl_r.fits—master flat_filter

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nfl_r.fits normalized flat_filterbbias substractedbobject_r1.fitsorb_object_r1.fitsnnormalisednobject_r1.fits aalignedaobject_r1.fitsccosmic reducedcobject_r1.fitsssummedsobject_r1.fitsuunit exposureuobject_r1.fitsscscaledscobject_r1.fitssksky substractedskobject_r1.fits

Spectroscopy:wobject.fitswavelength calibratedfobject.fitsflux calibrated

Regarding folder:1. floder name as yyyy_mm_dd2. for original data3. all preprocessing4. outside the current working.

03IRAF Commands (Before data reduction )

Hint & Summarise:Before starting reduction....what are things to be noted in mind.Depends which telescope data you are using..change the signal to noise ratio.....and gain....value asked in ....while 1.epar zerocombine—for bias2.epar flatcombine—for flat3.epar imcombinefor object at last only(after preprocessing individual frames )4.

epar display.....it should be fill = yes) scale image to fit display window

otherwise it will be without binning..it will show the bigger image.

While spectro reduction ...better to cut the unwanted portion.....means trimming...other wise unwanted

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lines will be produced...in corner side of the spectrum.

In spectro....disp command wont work.....only display ...will work.

*********************************************************************************

TO view the full details of one .fits file

>imhead <filename> l+ | page or)>imhead <filename> lo+

to bring control bar in the iraf terminal pressctrl+right clickin the cursor>e ........typing like this we can get the earlier commands

to come out or interupt: ctrl+c

Converting fts file to fits file .From the terminal[chrisphin@aries25 22mar07]$ wr2fits <imagename>Image info: image nameFilter: <filter Name>where wr2fits is an executable file....which is in the computer.written only for the image name andfilter for ARIES.

[chrisphin@aries25 22mar07]$ wr2fits bi*Totally are to be processedPlease enter the default parameters : Image info : bias Filter : none1 ) Input file: bi_1.fts outputfile: bi_1.fits2) Input file: bi_2.fts outputfile: bi_2.fits

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ob1.fits ,ob2.fits....if v you want to make a list then :

> ob *.fits >>jude> !emacs jude &

cl> show versionNOAO/IRAF V2.12.2EXPORT

cl>show printerlp

cl> refer photometry

cl> help [az]*

For saving the Graph:

:.snap epsflTo make a list :

suppose there are frames like.flr1.fits,flr2.fits...................flr9.fits

you wants to make a list (for bias subtraction..for all at a time...through epar ccdproc..then.)

>ls flr* >list

im> edisp aobject_r1.fits frame to be written into (1:4) (2): z1=1380.411 z2=1612.45im> display zs zr z1=1500 z2=3000image to be displayed (tn1156r01.fits): frame to be written into (1:4) (2): z1=1500. z2=3000.im> display zs zr z1=230 z2=900

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image to be displayed (tn1156r01.fits): ctn1156a01.fits frame to be written into (1:4) (2): 1z1=230. Z2=900.Where z1 be the the sky counts.And z2 be the object counts.Simply the range must be in betweeen these values.For the above command while displaying where the sky count shows the z1=<1500z2=some thing like 2350 to 2620....so it has given that z1=1500 z2=3000

while combining the images if you want to see the details on the screen itself, then give in the place.....

logfile =STDOUTthen you can see the output there itself.HINT:Always try to make the output file in the form of .imh (means leave automatically it will takethe extension of .imh)then the storage space you will get more .Then convert that into fits formatby the command “wfits”

cc> wfits mbi.imh FITS filename(s) (mbi): Image 1: mbi.imh > mbi.fits bias_img Size = 2048 x 2048 pixtype=real bitpix=32 blkfac=fixed scaling=none 3 Header 5826 Data logical (2880 byte) records writtenActually this imh file stores at /iraf/imdirs/chrisphin.So before take into another computer better tochange it into fits format.

About imexam:>imexam

go to the ds9 image....and placing the cursor on a star.press

afor statitics detailsrradial plotecontour plotc—coloumn plotlline plot

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w—logfile will close. while displaying the images if it fills the images full of window of ds9(SAO)then go to the display and change the below shown ( darken region) no to yes.now display it will be o.k. cc> epar display

PACKAGE = tv TASK = display image = image to be displayedframe = 1 frame to be written into(bpmask = BPM) bad pixel mask(bpdispl= none) bad pixel display (none|overlay|interpolate)(bpcolor= red) bad pixel colors(overlay= ) overlay mask(ocolors= green) overlay colors(erase = yes) erase frame(border_= no) erase unfilled area of window(select_= yes) display frame being loaded(repeat = no) repeat previous display parameters(fill = yes) scale image to fit display window(zscale = yes) display range of greylevels near median(contras= 0.25) contrast adjustment for zscale algorithm(zrange = yes) display full image intensity range(zmask = ) sample mask(nsample= 1000) maximum number of sample pixels to use(xcenter= 0.5) display window horizontal center(ycenter= 0.5) display window vertical center(xsize = 1.) display window horizontal size(ysize = 1.) display window vertical size(xmag = 1.) display window horizontal magnification(ymag = 1.) display window vertical magnification(order = 0) spatial interpolator order (0=replicate, 1=linea(z1 = ) minimum greylevel to be displayed(z2 = ) maximum greylevel to be displayed(ztrans = linear) greylevel transformation (linear|log|none|user)(lutfile= ) file containing user defined look up table(mode = ql)

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:wqFor trimming;PACKAGE = ccdred TASK = ccdprocimages = @list List of CCD images to correct(output = T//@list) List of output CCD images(ccdtype= ) CCD image type to correct(max_cac= 0) Maximum image caching memory (in Mbytes)(noproc = no) List processing steps only?

(fixpix = no) Fix bad CCD lines and columns?(oversca= no) Apply overscan strip correction?(trim = yes) Trim the image?(zerocor= no) Apply zero level correction?(darkcor= no) Apply dark count correction?(flatcor= no) Apply flat field correction?(illumco= no) Apply illumination correction?(fringec= no) Apply fringe correction?(readcor= no) Convert zero level image to readout correction?(scancor= no) Convert flat field image to scan correction?

(readaxi= line) Read out axis (column|line)(fixfile= ) File describing the bad lines and columns(biassec= ) Overscan strip image section(trimsec= [25:999,25:999]) Trim data section(zero = ) Zero level calibration image(dark = ) Dark count calibration image(flat = ) Flat field images(illum = ) Illumination correction images(fringe = ) Fringe correction images(minrepl= 1.) Minimum flat field value(scantyp= shortscan) Scan type (shortscan|longscan)(nscan = 1) Number of short scan lines

(interac= no) Fit overscan interactively?(functio= legendre) Fitting function(order = 1) Number of polynomial terms or spline pieces(sample = *) Sample points to fit

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(naverag= 1) Number of sample points to combine(niterat= 1) Number of rejection iterations(low_rej= 3.) Low sigma rejection factor(high_re= 3.) High sigma rejection factor(grow = 0.) Rejection growing radius(mode = ql)

if you want to be “ y ' section to be reamain then [x1:x2,*]then for apeture photometry small correction:

where in midas if you want use as the terminal for all the commands..then before command type $...ex:> $ls

For summing the subexposures images (for the same filter)Ex: imageu1.fits 15min }image u2.fits15min }imageu1.fits45min—imageu3.fits15min } The task is>epar imcombinePACKAGE = immatch TASK = imcombine

input = image*.fits List of images to combine* represents all the images with output = fnbhal.fits List of output images (combine= sum) Type of combine operation(rdnoise= 4.8) ccdclip: CCD readout noise (electrons)(gain = 1.22) ccdclip: CCD gain (electrons/DN):goOthers are all by default only change the above darkened.Note: Change the exposure time in imheader for the output

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04.Setting observatorycl>noaono>epar observatoryPACKAGE = noao TASK = observatory

command = set Command (set|list|images)obsid = ARIES Observatory to set, list, or image defaultimages = List of images(verbose= yes) Verbose output?

(observa= obspars) Observatory identification(name = ARIES) Observatory name(longitu= 280.514) Observatory longitude (degrees)(latitud= 29.36) Observatory latitude (degrees)(altitud= 1950.) Observatory altitude (meters)(timezon= 5.5) Observatory time zone(mode = ql)

override= obspars Observatory identification

:goObservatory identification (obspars):Using observatory parameters from observatory task# Observatory parameters for ARIES observatory = obspars timezone = 5.5 altitude = 1950. latitude = 29.36 longitude = 280.5140000000001 name = ARIES

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05. Setting Airmass for hct one prog has written it is /home/chrisphin/bin/airmass1 this will do by itself.

for that >noao>astutil>astheditas> astheditImages to be operated upon ( wobject.fits): File of commands (/home/chrisphin/bin/airmas1): 17.761111111111112006.193675691432453807.240046310.374161111111111.12053504889221

then check the imheader;as> imhead wobject.fits lo+

(in the last row it will join)

LONG = 281.0358LAT = 32.7795UT = '17:45:40'EP = 2006.19367569143JD = 2453807.2400463ST = '10:22:26.98'RAP = '12:27:53.73'DAP = '44:07:42.71'HA = 2.09076388888889AIRMASS = 1.12053504889221

before setting airmass confirm that respective observatory has been set.how to set it is given .as> setairmassInput images (csa104*.fits): fn*.fits

# Image UT middle effective begin middle end updated# SETAIRMASS: Observatory parameters for ARIES# latitude = 29.36 fn4449a1.fits 18:23:41.0 1.1303 1.1281 1.1303 1.1325 yes fn4449a2.fits 18:31:14.0 1.1439 1.1393 1.1439 1.1487 yes

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as> epar setairmassPACKAGE = astutil TASK = setairmass

images = nobj* Input images(observa= obspars) Observatory for images(intype = beginning) Input keyword time stamp(outtype= effective) Output airmass time stamp

(ra = ra) Right ascension keyword (hours)(dec = dec) Declination keyword (degrees)(equinox= epoch) Equinox keyword (years)(st = st) Local sidereal time keyword (hours)(ut = ut) Universal time keyword (hours)(date = dateobs) Observation date keyword(exposur= exptime) Exposure time keyword (seconds)(airmass= airmass) Airmass keyword (output)(utmiddl= utmiddle) Midobservation UT keyword (output)(scale = 750.) The atmospheric scale height(show = yes) Print the airmasses and midUT?

:go

06Basic Reduction

from terminal>xgterm.fedora&>ds9&

then from xgterm terminalchrisphin > cl NOAO PCIRAF Revision 2.12.2EXPORT Sun Jan 25 16:09:03 MST 2004 This is the EXPORT version of PCIRAF V2.12 supporting most PC systems.

Welcome to IRAF. To list the available commands, type ? or ??. To get detailed information about a command, type `help command'. To run a command or load a package, type its name. Type `bye' to exit a package, or `logout' to get out of the CL. Type `news' to find out what is new in the version of the system you are using. The following

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commands or packages are currently defined:

dataio. language. obsolete. softools. tables. dbms. lists. plot. stsdas. utilities. images. noao. proto. system. cl> noao artdata. digiphot. nobsolete. onedspec. astcat. focas. nproto. rv. astrometry. imred. observatory surfphot. astutil. mtlocal. obsutil. twodspec. no> im argus. crutil. echelle. iids. kpnocoude. specred. bias. ctioslit. generic. irred. kpnoslit. vtel. ccdred. dtoi. hydra. irs. quadred. im> cc badpiximage ccdmask flatcombine mkskyflat ccdgroups ccdproc mkfringecor setinstrument ccdhedit ccdtest mkillumcor zerocombine ccdinstrument combine mkillumflat ccdlist darkcombine mkskycor cc> ls

then go to the respective file.In the upcoming task commands consider only about the darken region others are all default

cc>epar zerocombinefor making master biasPACKAGE = ccdred TASK = zerocombine input = b*.fits List of zero level images to combineall bias images by * mark(output = mbias.fits) Output zero level name(combine= median) Type of combine operation(reject = none) Type of rejection(ccdtype= ) CCD image type to combine(process= no) Process images before combining?(delete = no) Delete input images after combining?(clobber= no) Clobber existing output image?(scale = none) Image scaling(statsec= ) Image section for computing statistics(nlow = 0) minmax: Number of low pixels to reject(nhigh = 1) minmax: Number of high pixels to reject

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(nkeep = 1) Minimum to keep (pos) or maximum to reject (neg)(mclip = yes) Use median in sigma clipping algorithms?(lsigma = 3.) Lower sigma clipping factor(hsigma = 3.) Upper sigma clipping factor(rdnoise= 5.3) ccdclip: CCD readout noise (electrons)(gain = 10) ccdclip: CCD gain (electrons/DN)(snoise = 0.) ccdclip: Sensitivity noise (fraction)(pclip = 0.5) pclip: Percentile clipping parameter(blank = 0.) Value if there are no pixels(mode = ql)

(if you are giving type of rejection is avgclip then no need of giving ccd parameters???correct it...this.)cc> imstat mbias* IMAGE NPIX MEAN STDDEV MIN MAX mbias.fits 1048576 1.949 0.9981 3. 7. mbias1.fits 1048576 1.934 0.8802 2. 6.(above mbias.fits is the combination of median and ccdclipmbias1.fits is the combination of median and none)

Jul 26 14:13: IMCOMBINE

combine = median, scale = none, zero = none, weight = none reject = minmax, nlow = 0, nhigh = 1 blank = 0. Images bias1.fits bias2.fits bias3.fits bias4.fits bias5.fits bias6.fits

Output image = mbias.fits, ncombine = 6

for substracting master bias from all the images use ccdproc command. or if you wants to do it one by onethen use imarith command>imarith inputimage – mbias.fits outputimage

>ls *.fits >>listJust to do all at one time make a list and do at one stroke.cc>epar ccdproc PACKAGE = ccdred

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TASK = ccdproc images = @list List of CCD images to correct(output = b//@list) List of output CCD images(ccdtype= ) CCD image type to correct(max_cac= 0) Maximum image caching memory (in Mbytes)(noproc = no) List processing steps only?(fixpix = no) Fix bad CCD lines and columns?(oversca= no) Apply overscan strip correction?(trim = no) Trim the image?(zerocor= yes) Apply zero level correction?(darkcor= no) Apply dark count correction?(flatcor= no) Apply flat field correction?(illumco= no) Apply illumination correction?(fringec= no) Apply fringe correction?(readcor= no) Convert zero level image to readout correction?(scancor= no) Convert flat field image to scan correction? (readaxi= line) Read out axis (column|line)(fixfile= ) File describing the bad lines and columns(biassec= ) Overscan strip image section(trimsec= ) Trim data section(zero = mbias.fits) Zero level calibration image(dark = ) Dark count calibration image(flat = ) Flat field images(illum = ) Illumination correction images(fringe = ) Fringe correction images(minrepl= 1.) Minimum flat field value(scantyp= shortscan) Scan type (shortscan|longscan)(nscan = 1) Number of short scan lines(interac= no) Fit overscan interactively?(functio= legendre) Fitting function(order = 1) Number of polynomial terms or spline pieces(sample = *) Sample points to fit (naverag= 1) Number of sample points to combine(niterat= 1) Number of rejection iterations(low_rej= 3.) Low sigma rejection factor(high_re= 3.) High sigma rejection factor(grow = 0.) Rejection growing radius(mode = ql)

:go

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then running as...sa104b07.fits: Jul 26 14:43 Zero level correction image is mbias.fitssa104r01.fits: Jul 26 14:43 Zero level correction image is mbias.fits

then the result will come with substracted with the name of b<filename>.fits.ex: bobject_r1.fits

now the images are all bias substracted...from master bias.fits.cc> epar flatcombinedo it for same filter images alone in one for flat combine using thisPACKAGE = ccdred TASK = flatcombine

input = bflat_r* List of flat field images to combinebias subtracted all flat images of oneparticular filter

(output = mfl_r.fits) Output flat field root name(combine= median) Type of combine operation(reject = avsigclip) Type of rejection(ccdtype= ) CCD image type to combine(process= no) Process images before combining?(subsets= no) Combine images by subset parameter?(delete = no) Delete input images after combining?(clobber= no) Clobber existing output image?(scale = mode) Image scaling(statsec= ) Image section for computing statistics(nlow = 1) minmax: Number of low pixels to reject(nhigh = 1) minmax: Number of high pixels to reject(nkeep = 1) Minimum to keep (pos) or maximum to reject (neg)(mclip = yes) Use median in sigma clipping algorithms?(lsigma = 3.) Lower sigma clipping factor(hsigma = 3.) Upper sigma clipping factor(rdnoise= 5.3) ccdclip: CCD readout noise (electrons)(gain = 10) ccdclip: CCD gain (electrons/DN)(snoise = 0.) ccdclip: Sensitivity noise (fraction)(pclip = 0.5) pclip: Percentile clipping parameter(blank = 1.) Value if there are no pixels(mode = ql)

;go

Jul 26 14:57: IMCOMBINE

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combine = median, scale = mode, zero = none, weight = none reject = avsigclip, mclip = yes, nkeep = 1 lsigma = 3., hsigma = 3. blank = 1. Images Exp Mode Scale bflata1.fits 200.0 2408. 2.217 bflata2.fits 200.0 7314. 0.730 bflata3.fits 70.0 6295. 0.848

Output image = mfla.fits, ncombine = 3

like that do it individually for all the different filters.

For normalisation:cc> imstat mfl_r.fits # IMAGE NPIX MEAN STDDEV MIN MAX mfla.fits 1048576 5411. 173.7 1.957 8428.cc> imarith mfl_r.fits / 5411. nfl_r.fits (like that do it for other filter.)

cc> imarith bobject_r1.fits / nfl_r.fits nobject_r1.fits

(like that do it for all with respect to their filter flat)

cc>ls bn* >list2cc> imarith @list2 / nflr.fits f//@list2

Hint: Repalcing bad pixelcc>epar imreplacePACKAGE = imutil TASK = imreplace

images = bflat_r* Images to be editedvalue = 1. Replacement pixel value(imagina= 0.) Imaginary component for complex(lower = 0.) Lower limit of replacement window(upper = INDEF) Upper limit of replacement window(radius = 0.) Replacement radius

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(mode = ql)

:go

OR –if you wants to replace particular portion open the image and note down the that particularcoordinates

replacing bad pixel...........cc> disp test_5430.fits 1z1=1.380593 z2=1.359507cc>imreplace test_5430.fits[1051:1055,955:959] 3.5cc>epar imreplacePACKAGE = imutil TASK = imreplace

images = test_5430.fits[1051:1055,955:959] Images to be editedvalue = 3.5 Replacement pixel value(imagina= 0.) Imaginary component for complex(lower = INDEF) Lower limit of replacement window(upper = INDEF) Upper limit of replacement window(radius = 0.) Replacement radius(mode = ql)

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07Alignment

first display the respective frame....in ds9.alway stry to choose the red filter frame as are referenceone.cc> disp nobject_r1.fitsframe to be written into (1:16) (2):1z1=1.951634 z2=15.75021

to create an file type :cc> epar imexamPACKAGE = tv TASK = imexamine input = nobject_r1.fits images to be examined(output = ) output root image name(ncoutpu= 101) Number of columns in image output(nloutpu= 101) Number of lines in image outputframe = 1 display frameimage = image name(logfile= al.co) logfile(keeplog= yes) log output results

:goLog file al.co open

Then in image selct some number of stars by placing 'cursor 'in the middle of a star and press 'a' ....it will give the details of stars in xgterm.the peak value should be within the range of 100028,000. The 28,000 value is with respect to ouraries.then “q”cc>emacs al.cothen delete all other parameter except (the darken region) colum and line cordinates.# [1] nobject_r1.fits hz44# COL LINE COORDINATES R MAG FLUX SKY PEAK E PA BETA ENCLOSED MOFFAT DIRECT 282.88 393.49 282.88 393.49 9.88 15.82 4713. 5.721 318.2 0.20 88 4.08 3.26 3.27 3.29 286.26 438.66 286.26 438.66 10.73 17.45 1044. 5.796 61.75 0.11 39 6.84 3.04 4.01 3.60 420.94 550.00 420.94 550.00 10.52 12.95 66003. 6.676 4326. 0.26 88 3.00 3.13 3.50 3.50 462.09 658.93 462.09 658.93 10.43 15.96 4136. 5.934 259. 0.03 79 3.00 3.11 3.48 3.48 507.39 741.35 507.39 741.35 11.09 16.68 2137. 6.053 134.1 0.10 57 13.0 3.25 3.57 3.72 601.68 613.98 601.68 613.98 11.82 17.62 898.9 5.984 48.34 0.17 67 12.0 3.56 4.00 3.97

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then it becomes

282.88 393.49 286.26 438.66 420.94 550.00 462.09 658.93 507.39 741.35 601.68 613.98

then save it and close come out.then display the another frame which is going to be aligned wrt reference.cc> display nobject_r2.fits 2z1=0.9973257 z2=15.23859

cc> tvmarkDefault frame number for display (:16) (2): Input coordinate list (al.co):

cc> imexamLog file al.co open

then selct the respective stars in order. then quit from the imagecc> emacs al.cothen the emacs will open like 282.88 393.49 286.26 438.66 420.94 550.00 462.09 658.93 507.39 741.36 601.68 613.98 # [1] nobject_r1.fits hz44# COL LINE COORDINATES R MAG FLUX SKY PEAK E PA BETA ENCLOSED MOFFAT DIRECT 283.33 396.57 283.33 396.57 10.60 15.85 4571. 5.693 303.9 0.21 87 3.00 3.07 3.53 3.53 286.75 441.81 286.75 441.81 11.76 17.64 881.7 5.672 58.21 0.77 27 10.4 3.22 3.79 3.95 421.38 553.07 421.38 553.07 10.65 12.95 65882. 5.804 4333. 0.26 88 22.4 3.11 3.55 3.56 462.56 662.05 462.56 662.05 11.02 16.02 3906. 5.856 248.3 0.43 79 24.3 3.25 3.65 3.67 507.83 744.34 507.83 744.34 10.76 16.75 1994. 6.031 138.5 0.32 75 12.4 3.10 3.48 3.60 602.13 617.12 602.13 617.12 10.66 17.83 735.4 5.956 52.11 52.6 78 5.65 3.11 3.52 3.54

then delete the unwanted make it like the bottom one.....(by taking only the darkened part shownabove)

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282.88 393.49 283.33 396.57 286.26 438.66 286.75 441.81 420.94 550.00 421.38 553.07 462.09 658.93 462.56 662.05 507.39 741.36 507.83 744.34 601.68 613.98 602.13 617.12

and save it.For cut> (ctrl+x) + rkFor paste >(ctrl+x) + rycc> epar geomap

PACKAGE = immatch TASK = geomap input = al.co The input coordinate filesdatabase= al.co_db The output database filexmin = 1. Minimum x reference coordinate valuexmax = 1024. Maximum x reference coordinate valueymin = 1. Minimum y reference coordinate valueymax = 1024. Maximum y reference coordinate value(interac= no) Fit transformation interactively ?

:goCoordinate list: al.co Transform: al.co Results file: tobject_r2.fitsCoordinate mapping status X fit ok. Y fit ok. Xin and Yin fit rms: 0.01747025 0.04828498Coordinate mapping parameters Mean Xref and Yref: 426.8733 566.07 Mean Xin and Yin: 427.33 569.16 X and Y shift: 0.4870407 3.221664 (xin yin) X and Y scale: 0.9999283 0.9994867 (xin / xref yin / yref) X and Y axis rotation: 359.979 0.000 (degrees degrees)cc> epar geotranPACKAGE = immatch TASK = geotran

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input = nobject_r2.fits Input dataoutput = aobject_r2.fits Output datadatabase= al.co_db Name of GEOMAP database filetransfor= al.co Names of coordinate transforms in database file

Transforming image nobject_r2.fits to image aobject_r2.fits Using transform al.co in database al.co_db

THAT IS IT HAVE FUN.PACKAGE = tv TASK = tvmarkframe = 1 Default frame number for displaycoords = al.co Input coordinate list(logfile= ) Output log file(autolog= no) Automatically log each marking command(outimag= ) Output snapped image(deletio= ) Output coordinate deletions list (command= ) Image cursor: [x y wcs] key [cmd](mark = circle) The mark type(radii = 0) Radii in image pixels of concentric circles(lengths= 0) Lengths and width in image pixels of concentric (font = raster) Default font(color = 255) Gray level of marks to be drawn(label = no) Label the marked coordinates(number = yes) Number the marked coordinates(nxoffse= 0) X offset in display pixels of number(nyoffse= 0) Y offset in display pixels of number(pointsi= 3) Size of mark type point in display pixelsMore

after alignment check by displaying all the images into different frames.then pressing center in the ds9 display.(then only everthing will be according to centre it willdisplay)

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08Cosmic ray reduction through MIDAS

Go to the respective file.where the reducing fits files contains.

chrisphin>inmidasESOMIDAS version 06FEBpl1.0 on PC/LinuxMidas 015>Midas 015> set/con daophotonly once at the time of starting

***** DAOPHOT application package version April 1991 enabled *****commands available:ALLSTAR/DAOPHOT Do simultaneous multipleprofilefittingDAOPHOT/DAOPHOT Do stellar photometry in 2dimensional imagesDAOMID/DAOPHOT Convert DAOPHOT tables to MIDAS tablesMIDDAO/DAOPHOT Convert MIDAS tables to DAOPHOT tables

Midas 016> indisk/fits aobjectr_1.fits aobject_r1.bdf

no CDELTi nor CDi_j matrix found... STEPi set to 1.0FITS file: tfbn4449b1.fits converted to: tfbn4449b1.bdf

(Midas 020> help fil/cosmicFILTER/COSMIC )

Midas 021> daophotRevised version W A R N I N G

This version of DAOPHOT can be used for frames with a maximum size of 4100 * 4100 (= 16810000) pixels. In case your frame is larger than this value, DAOPHOT will not be able to process it. In such case, please contact your local MIDAS support person. READ NOISE (ADU; 1 frame) = 5.00 GAIN (e/ADU; 1 frame) = 10.00 OW GOOD DATUM (in sigmas) = 7.00 HIGH GOOD DATUM (in ADU) = 30000.00 FWHM OF OBJECT = 2.50 THRESHOLD (in sigmas) = 4.00 LS (LOW SHARPNESS CUTOFF) = 0.20 HS (HIGH SHARPNESS CUTOFF) = 1.00 LR (LOW ROUNDNESS CUTOFF) = 1.00 HR (HIGH ROUNDNESS CUTOFF) = 1.00

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WATCH PROGRESS = 1.00 FITTING RADIUS = 2.00 PSF RADIUS = 15.00 VARIABLE PSF = 0.00 FRACTIONALPIXEL EXPANSION = 0.00 ANALYTIC MODEL PSF = 1.00 EXTRA PSF CLEANING PASSES = 5.00 PERCENT ERROR (in %) = 0.75 PROFILE ERROR (in %) = 5.00

Command: at aobject_r1 ngc 4449

Picture size: 1024 1024 Command:sky

Approximate sky value for this frame = 111.2 Standard deviation of sky brightness = 3.58

Command: exit(0.53=5.3/10 ie...readout noise in ADU.)

Midas 025> fil/cosmic aobject_r1.bdf cobject_r1.bdf 111.2,10,0.53,4,2 (fil/cosmic aobject_r1.bdf cobject_r1.bdf skyvalue,Gain,Readout Noise/Gain,4,2 )Beginning of the median filterwe process frame in 2 chunks ...expanding frame Th, 18 May 2006 14:37:08working on chunk 1 Th, 18 May 2006 14:37:09working on chunk 2 Th, 18 May 2006 14:37:09Beginning of the cosmic rays removal

Midas 026> outdisk/fits cobject_r1.bdf cobject_r1.fitsFITS file cfbn4449b1.fits will have 1 extensionscfbn4449b1.bdf written to FITS file cfbn4449b1.fits( To check whether mistakenly some stars are deleted are not.This mask.fits give only the removedpart...so from that by plotting Intensity profile (pressing 's'from Ds9)we can easily find out)Midas 027> fil/cosmic aobject_r1.bdf cobject_r1.bdf 111.2,10,0.53,4,2 mask.bdfBeginning of the median filterwe process frame in 2 chunks ...expanding frame Th, 18 May 2006 14:38:03

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working on chunk 1 Th, 18 May 2006 14:38:03working on chunk 2 Th, 18 May 2006 14:38:03Beginning of the cosmic rays removalMidas 028> outdisk/fits mask.bdf mask.fitsFITS file mask.fits will have 1 extensionsmask.bdf written to FITS file mask.fits

Hints:For getting help Midas 020> help fil/cosmic FILTER/COSMIC )

While staring for the next one no need to type again>set/con daophot

Instead directly start from indisk/fits ......................Problem in midas:Midas 016> indisk/fits TAfe34_a2.fits TAfe34_a2.bdfWarning: <COMMENT1> of invalid type not storedWarning: <COMMENTX> of invalid type not storedrotlong = 6.283185, rotlat = 0.000000 axes not orthogonal!FITS file: TAfe34_a2.fits converted to: Tafe34_a2.bdf

Midas 018> help fil/cosmicFILTER/COSMIC 21NOV1991 PM,MR

Purpose: Remove cosmic ray events on a single CCD image and replace them by a local median value.Syntax: FILTER/COSMIC inframe outframe sky,gain,ron,[ns,rc] [mask] inframe = raw input frame outframe = output frame sky,gain,ron,ns,rc = sky level (sky), inverse gain factor (e/ADU) (gain), readoutnoise (in ADU) (ron), threshold for the detection of cosmic rays (ns), and critical ratio for discrimination of objects and cosmic rays (rc). The detection threshold is in units of the theoretical noise sigma of each pixel; it's default value is 4. The default for `rc' is 2.

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mask = name of an optional frame containing the value 1 for cosmic rays and 0 for all other pixels.

Note: a) The algorithm works as follows: 1. The input image is filtered in the following way: FILTER/MEDIAN inframe middumma 1,1,0.0 NA For LongSlit spectra of extended sources, the algorithm may be

hit return to continue, 'q' + return to quit Midas 018> help fil/cosmicFILTER/COSMIC 21NOV1991 PM,MR

Purpose: Remove cosmic ray events on a single CCD image and replace them by a local median value.Syntax: FILTER/COSMIC inframe outframe sky,gain,ron,[ns,rc] [mask] inframe = raw input frame outframe = output frame sky,gain,ron,ns,rc = sky level (sky), inverse gain factor (e/ADU) (gain), readoutnoise (in ADU) (ron), threshold for the detection of cosmic rays (ns), and critical ratio for discrimination of objects and cosmic rays (rc). The detection threshold is in units of the theoretical noise sigma of each pixel; it's default value is 4. The default for `rc' is 2. mask = name of an optional frame containing the value 1 for cosmic rays and 0 for all other pixels.Note: a) The algorithm works as follows: 1. The input image is filtered in the following way: FILTER/MEDIAN inframe middumma 1,1,0.0 NA For LongSlit spectra of extended sources, the algorithm may be

more efficient if the median filter works only along the slit. 2. The input image is compared with the filtered image. All pixels with an intensity I greater than Im+ns*sigma are suspicious and may be cosmic rays (Im is the filtered intensity of a pixel and sigma is given by: sigma**2 = ron**2+I/gain).

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3. All suspicious pixels are grouped into sets of contiguous points. In each of these sets, the pixel with the maximum intensity Imax is selected. If (Imaxsky) is greater than rc*(Iaversky), Iaver being an average of the intensities of the first eight neighbours of that pixel, the whole set of points is considered as a cosmic ray event. 4. The intensities of the pixels affected by cosmic rays are replaced by a median value calculated over the nearest neighbours of the group to which they belong. b) In many situations, rc is the most critical parameter and requires careful finetuning. If it is choosen too small, small sources such as stars may be affected. If rc is too large, the filter may not remove weak partical hits superimposed to reasonably well exposed extended sources.See also: FILTER/MEDIANExamples: FILTER/COSMIC ccd ccdclean 150,1,4,4,2.3 cosmask Apply cosmic filtering to image `ccd.bdf' and store result frame

hit return to continue, 'q' + return to quit as `ccdclean.bdf'; save a 0/1 mask in `cosmask.bdf'.Midas 019> FILTER/COSMIC 21NOV1991 PM,MREnter SKY,G,RON,NS,RC:

33


09Cosmic ray reduction through IRAFcc> disp aobject_r1.fitsframe to be written into (1:16) (1): z1=102.8171 z2=133.1152cc> imexam

Then in Ds 9 image select isolated field and press 'm' cc> imexam (sky)# SECTION NPIX MEAN MEDIAN STDDEV MIN MAX [684:688,774:778] 25 109.7 110. 1.995 106.3 113.8 [112:116,382:386] 25 112.7 112.8 2.597 108.5 117.1 [244:248,210:214] 25 111.5 111.6 2.64 106. 116.7 [276:280,114:118] 25 111.7 111.6 1.704 108.7 115.1 [390:394,72:76] 25 110.4 110.5 2.229 104.2 114.3 [768:772,118:122] 25 110.2 110. 2.837 105.4 118.1 [906:910,148:152] 25 110.4 110.4 3.277 104.8 117.3 [960:964,638:642] 25 109.7 109.1 1.615 107.2 112.3 [908:912,866:870] 25 109.5 109.6 2.201 104.4 113.9 [44:48,832:836] 25 112.5 112.8 1.708 109.1 115.2cc> crutil cosmicrays crcombine crfix crmedian craverage credit crgrow crnebula cr> epar cosmicinput = aobject_b1.fits List of images in which to detect cosmic raysoutput = ctobject_b1.fits List of cosmic ray replaced output images (optio(crmasks= ) List of bad pixel masks (optional)

(thresho= 11.) Detection threshold above mean

:goaobject_b1.fits Review parameters for a particular image? (no|yes|NO|YES) (yes): yes

Then the figure will come.

* here the threshold is mean of standard deviation multiply with 5.here it is 2.2*5=11

then the figure will come place the cursor over any particular point and press "s"then the plot will come.

1.if the plot is so sharp (peak) then it must be cosmic ray.

34


1.if it is blended (following gaussian distribution)....then it is a star.

press "s"see the plottingcome back by pressing "s"then delete "d"for undelete “u”then for quit “q”also flux ratio also important.this is nothing but.....the ratio between the cosmic ray flux and sky flux ....normally this value ....

10Apeture Photometry

first make a coordinate file by selecting 10 or 15 stars....here i have selected first 5standardstars..then 3 faint stars..and made a file in the name of ' co ' like that.>epar imexam

(logfile= co) logfile(keeplog= yes) log output results:golog file open(Now select the stars ...it will be in the file named ' co ' )>imexamSA 104MEAN OF MEAN OF FWHM(Direct)STD DEV (for the five standard stars)(for the darken region)(by pressing 'a')(by pressing 'm')r01 3.4 2.6

like that for each frame find out the value through imexam command.and make a note of it .

cl> noao artdata. digiphot. mtlocal. observatory surfphot. astrometry. focas. nobsolete. onedspec. twodspec. astutil. imred. nproto. rv. no> digi apphot. daophot. photcal. ptools. di> daophot

35


addstar daotest nstar pexamine psf allstar datapars@ pcalc pfmerge psort centerpars@ findpars@ pconcat phot pstselect daoedit fitskypars@ pconvert photpars@ seepsf daofind group pdump prenumber setimpars daopars@ grpselect peak pselect substar

da> epar photPACKAGE = apphot TASK = phot

image = cobject_r1.fits The input image(s)skyfile = The input sky file(s)(coords = co) The input coordinate files(s) (default: image.coo.?)(output = default) The output photometry file(s) (default: image.mag.?)(plotfil= ) The output plots metacode file(datapar= ) Data dependent parameters(centerp= ) Centering parameters(fitskyp= ) Sky fitting parameters(photpar= ) Photometry parameters(interac= no) Interactive mode ?

in the above darken region place the cursor and type :e Then for datapar

da> epar phot

PACKAGE = daophot TASK = datapars

(scale = 1.) Image scale in units per pixel(fwhmpsf= 3.74) FWHM of the PSF in scale units(emissio= yes) Features are positive ?(sigma = 0.0015) Standard deviation of background in countssigma value(datamin= 0.2375) Minimum good data valuesky5*sigma(datamax= 28000.) Maximum good data valueSaturation level ...(noise = poisson) Noise model(ccdread= ) CCD readout noise image header keyword

36


(gain = ) CCD gain image header keyword(readnoi= 5.3) CCD readout noise in electrons(epadu = 10.) Gain in electrons per count(exposur= ) Exposure time image header keyword(airmass= ) Airmass image header keyword(filter = ) Filter image header keyword(obstime= ) Time of observation image header keyword(itime = 1.) Exposure time(xairmas= INDEF) Airmass

:qPACKAGE = daophot TASK = centerpars

(calgori= none) Centering algorithm(cbox = 6.44) Centering box width in scale units2*3.74 ie..2*FWHM(cthresh= 0.) Centering threshold in sigma above background(minsnra= 1.) Minimum signaltonoise ratio for centering algo(cmaxite= 10) Maximum iterations for centering algorithm(maxshif= 1.) Maximum center shift in scale units(clean = no) Symmetry clean before centering(rclean = 1.) Cleaning radius in scale units(rclip = 2.) Clipping radius in scale units(kclean = 3.) Ksigma rejection criterion in skysigma(mkcente= no) Mark the computed center(mode = ql)

:q PACKAGE = daophot TASK = fitskypars

(salgori= mode) Sky fitting algorithmconstantfor knots.default for others.(annulus= 12.88) Inner radius of sky annulus in scale units—4 to 5times FWHM for stars (dannulu= 5) Width of sky annulus in scale units5(interm of pixel i think)for stars(skyvalu= 0.) User sky value(smaxite= 10) Maximum number of sky fitting iterations(sloclip= 0.) Lower clipping factor in percent(shiclip= 0.) Upper clipping factor in percent

37


(snrejec= 50) Maximum number of sky fitting rejection iteratio(sloreje= 3.) Lower Ksigma rejection limit in sky sigma(shireje= 3.) Upper Ksigma rejection limit in sky sigma(khist = 3.) Half width of histogram in sky sigma(binsize= 0.1) Binsize of histogram in sky sigma(smooth = no) Boxcar smooth the histogram(rgrow = 0.) Region growing radius in scale units(mksky = no) Mark sky annuli on the display(mode = ql)

What? choose: |median|mode|centroid|gauss|crosscor|ofilter|histplot|radplot|co ESC? for HELPnstant|file|mean|

then for the knots....it differs...(only for fitskypars)..only this fitskypars nothing else.

PACKAGE = daophot TASK = fitskypars

(salgori= constant) Sky fitting algorithm(annulus= 0.) Inner radius of sky annulus in scale unitsfor knots (dannulu= 0.) Width of sky annulus in scale unitsfor knots(skyvalu= 0.15) User sky value(smaxite= 10) Maximum number of sky fitting iterations(sloclip= 0.) Lower clipping factor in percent(shiclip= 0.) Upper clipping factor in percent(snrejec= 50) Maximum number of sky fitting rejection iterations(sloreje= 3.) Lower Ksigma rejection limit in sky sigma(shireje= 3.) Upper Ksigma rejection limit in sky sigma(khist = 3.) Half width of histogram in sky sigma(binsize= 0.1) Binsize of histogram in sky sigma(smooth = no) Boxcar smooth the histogram(rgrow = 0.) Region growing radius in scale units(mksky = no) Mark sky annuli on the display(mode = ql)

:q

da> disp zs zr z1=.1 z2=1

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image to be displayed (nca_sr.fits): frame to be written into (1:4) (1): z1=0.1 z2=1.

While doing aperture for knots check from the1.vector plot(wher vector plot shows the total diameter ..but take only the radius)2.from the fluxfluctuationn in the flux....sudden rise and fall on the flux.3.from magnitude error.

PACKAGE = apphot TASK = photpars

(weighti= constant) Photometric weighting scheme for wphot(apertur= 10:20:.5) List of aperture radii in scale units(2FWHM:4FWHM:Interval)(zmag = 25.) Zero point of magnitude scale (start:end:interval)(mkapert= no) Draw apertures on the display(mode = ql)

Darken region explains :10—initial(FWHM)...20final radius(4FWHM)..5interval

:qthen from the main....phot pakage

:go

Centering algorithm (centroid) (CR or value): (just type enter for all ) New centering algorithm: centroidCentering box width in scale units (5.) (CR or value): New centering box width: 5. scale units 5. pixelsSky fitting algorithm (centroid) (CR or value): Sky fitting algorithm: centroidInner radius of sky annulus in scale units (20.) (CR or value): New inner radius of sky annulus: 20. scale units 20. pixelsWidth of the sky annulus in scale units (10.) (CR or value): New width of the sky annulus: 10. scale units 10. pixelsFile/list of aperture radii in scale units (10:20:.5) (CR or value): Aperture radius 1: 10. scale units 10. pixels

Aperture radius 2: 10.5 scale units 10.5 pixels Aperture radius 3: 11. scale units 11. pixels Aperture radius 4: 11.5 scale units 11.5 pixels Aperture radius 5: 12. scale units 12. pixels

39


Aperture radius 6: 12.5 scale units 12.5 pixels Aperture radius 7: 13. scale units 13. pixels Aperture radius 8: 13.5 scale units 13.5 pixels Aperture radius 9: 14. scale units 14. pixels Aperture radius 10: 14.5 scale units 14.5 pixels Aperture radius 11: 15. scale units 15. pixels Aperture radius 12: 15.5 scale units 15.5 pixels Aperture radius 13: 16. scale units 16. pixels Aperture radius 14: 16.5 scale units 16.5 pixels Aperture radius 15: 17. scale units 17. pixels Aperture radius 16: 17.5 scale units 17.5 pixels Aperture radius 17: 18. scale units 18. pixels Aperture radius 18: 18.5 scale units 18.5 pixels Aperture radius 19: 19. scale units 19. pixels Aperture radius 20: 19.5 scale units 19.5 pixels Aperture radius 21: 20. scale units 20. pixelsStandard deviation of background in counts (1.3) (CR or value): New standard deviation of background: 1.3 countsMinimum good data value (INDEF) (CR or value): New minimum good data value: INDEF countsMaximum good data value (28000.) (CR or value): New maximum good data value: 28000. counts

then it has been created one file as cobject_r1.fits.mag.1 by default.open and check it for which aperture it has constant value.and take that aperture value(example:19) put it into the coming ...>!vi cobject_r1.fits.mag.1 csa104b04.fits 351.540 867.290 1 co 1 \ 351.575 867.344 0.035 0.054 0.015 0.019 0 NoError \ 40.63198 1.279863 0.4462133 1562 9 0 NoError \ 1. INDEF INDEF INDEF \ 10.00 21848.62 314.3839 9074.581 15.105 0.012 0 NoError *\ 10.50 23208.14 346.9878 9109.336 15.101 0.012 0 NoError *\ 11.00 24588.55 380.2554 9138.025 15.098 0.012 0 NoError *\ " " 17.50 48452.44 962.6317 9338.808 15.074 0.013 0 NoError *\ 18.00 50711.02 1017.86 9353.36 15.073 0.013 0 NoError *\ 18.50 53070.39 1075.453 9372.596 15.070 0.013 0 NoError *\ 19.00 55497.81 1134.713 9392.172 15.068 0.013 0 NoError *\ 19.50 57950.38 1194.741 9405.702 15.068 0.013 0 NoError *\

here you can see the the difference in 19th aperture onwards (darken region)become constant. itmeans that the star is ending and sky is starting.that is the value we want.Hint:if the output somewhare gives INDEF and BAD PIXELS..then reduce the DATAMIN value ..yet..now giving the output it will be fine. ap> epar phot

40


then place that value in .....photmetry prameters...then execute new file has been created.(weighti= constant) Photometric weighting scheme for wphot(apertur= 19) List of aperture radii in scale units(zmag = 25.) Zero point of magnitude scale(mkapert= no) Draw apertures on the display(mode = ql)

:q:go

After that simply type enter …..enter

Centering algorithm (centroid) (CR or value): New centering algorithm: centroidCentering box width in scale units (5.) (CR or value): New centering box width: 5. scale units 5. pixelsSky fitting algorithm (centroid) (CR or value): Sky fitting algorithm: centroidInner radius of sky annulus in scale units (20.) (CR or value): New inner radius of sky annulus: 20. scale units 20. pixelsWidth of the sky annulus in scale units (10.) (CR or value): New width of the sky annulus: 10. scale units 10. pixelsFile/list of aperture radii in scale units (19) (CR or value): Aperture radius 1: 19. scale units 19. pixelsStandard deviation of background in counts (1.3) (CR or value): New standard deviation of background: 1.3 countsMinimum good data value (INDEF) (CR or value): New minimum good data value: INDEF countsMaximum good data value (28000.) (CR or value): New maximum good data value: 28000. count

new file name as...... cobject_r1.fits.mag.2

Now all the frames with the extension of .mag.2 is last one.collect all the file like this and edit itmake one file like ' mag ' with only needed parameters instead of all.through the command...

ap>epar txdumpPACKAGE = apphot TASK = txdumptextfile= *.mag.2 Input apphot/daophot text database(s)fields = ID,XCENTER,YCENTER,MAG,MERR,IMAGE,RAPERT,FLUX Fields to be extractedexpr = yes Boolean expression for record selection(headers= no) Print the field headers ?

41


(paramet= yes) Print the parameters if headers is yes ?(mode = ql) Mode of task

ap> txdump >magInput apphot/daophot text database(s) (*.mag.2): Fields to be extracted (ID,XCENTER,YCENTER,MAG,MERR,IMAGE,AIRMASS): Boolean expression for record selection (yes): ap> vi mag 1 351.556 867.093 14.467 0.011 csa104r01.fits 1.14342 364.319 688.529 12.815 0.004 csa104r01.fits 1.14343 401.578 604.448 13.608 0.007 csa104r01.fits 1.1434

(then the file is look like above mentioned where the last one is AIRMASShere airmass includedafter that manually)

Then open the terminal go to that file.cosmic > emacs mag& (this & symbol allowed to open two emacs windows )[3] 67941 351.529 867.175 14.850 0.015 csa104b02.fits 1.1467 2 364.414 688.483 12.978 0.005 csa104b02.fits 1.14673 401.631 604.402 14.223 0.009 csa104b02.fits 1.14674 511.751 492.538 15.646 0.025 csa104b02.fits 1.1467 5 263.457 436.599 15.279 0.019 csa104b02.fits 1.1467 6 855.151 553.466 INDEF INDEF csa104b02.fits 1.1467 7 943.576 663.904 11.166 0.002 csa104b02.fits 1.1467 8 612.870 812.539 14.962 0.016 csa104b02.fits 1.1467 9 745.028 914.030 14.606 0.013 csa104b02.fits 1.1467 10 844.448 691.592 15.543 0.024 csa104b02.fits 1.1467 1 351.498 868.058 15.001 0.013 csa104b03.fits 1.58422 364.394 689.294 13.147 0.005 csa104b03.fits 1.5842 3 401.589 605.307 14.345 0.009 csa104b03.fits 1.5842 4 511.650 493.542 15.734 0.019 csa104b03.fits 1.5842 """"" """" """"" """""" '''''

cosmic > emacs magb1&[4] 67951 14.850 0.015 csa104b02.fits 1.14671 15.001 0.013 csa104b03.fits 1.58421 15.068 0.013 csa104b04.fits 1.70201 15.217 0.014 csa104b05.fits 1.84601 15.410 0.017 csa104b06.fits 2.07811 15.478 0.019 csa104b07.fits 2.2980

(like this open two emacs and from the main (mag) take only the one particular star one

42


particular filter all frames(magb1)as shown above. or the simple command is from the terminal go to the respective file and type ......cosmic > awk '{if($1==2) print ($1,$4,$5,$6,$7)}' mag2 12.978 0.005 csa104b02.fits 1.14672 13.147 0.005 csa104b03.fits 1.58422 13.232 0.005 csa104b04.fits 1.70202 13.349 0.005 csa104b05.fits 1.84602 13.512 0.006 csa104b06.fits 2.07812 13.620 0.006 csa104b07.fits 2.29802 12.815 0.004 csa104r01.fits 1.14342 12.813 0.004 csa104r02.fits 1.15412 12.897 0.004 csa104r03.fits 1.51462 12.930 0.004 csa104r04.fits 1.66222 13.133 0.005 csa104r05.fits 1.79882 13.168 0.005 csa104r06.fits 1.94452 13.226 0.005 csa104r07.fits 2.22432 12.568 0.004 csa104v01.fits 1.14162 12.568 0.004 csa104v02.fits 1.15052 13.366 0.005 csa104v03.fits 1.54062 12.776 0.004 csa104v04.fits 1.76192 12.889 0.004 csa104v05.fits 1.90122 12.960 0.004 csa104v06.fits 2.15442 13.017 0.005 csa104v07.fits 2.3898

then it will list out the 2nd stars of all the frames and filter.as shown above.thencosmic > emacs magb2&[1] 10224cosmic > emacs magv2&[2] 10225[1] Done emacs magb2cosmic > emacs magr2&[3] 10226[2] Done emacs magv2

copy and paste the respective files.into this.then plotting the graph through the terminal and get the cofficient

This gnuplot type from the terminal where you wants to workcosmic > gnuplot G N U P L O T Version 4.0 patchlevel 0 last modified Thu Apr 15 14:44:22 CEST 2004 System: Linux 2.6.91.667smp

43


Copyright (C) 1986 1993, 1998, 2004 Thomas Williams, Colin Kelley and many others

This is gnuplot version 4.0. Please refer to the documentation for command syntax changes. The old syntax will be accepted throughout the 4.0 series, but all save files use the new syntax. Type `help` to access the online reference manual. The gnuplot FAQ is available from http://www.gnuplot.info/faq/

Send comments and requests for help to <gnuplot[email protected]> Send bugs, suggestions and mods to <gnuplot[email protected]>Terminal type set to 'x11'After inside the gnuplot if you want to list out the files to see then typegnuplot>!lsgnuplot>plot " magv1" u 5:2 plot”datafile”using coloum no in x:y

then the plotted graph will come.using the data magv1 colum no: 5 in x axis and colum no 2 inyaxis.nothing but in the x axis AIRMASS in yaxis MAGNITUDEFor saving the plotgnuplot>set term post gnuplot>set output “filename.ps”gnuplot>pl “data_filename” gnuplot> y(x)=m*x+cgnuplot> fit y(x) "magv1" u 5:2 via m,cthen in the terminal details will come .Iteration 0WSSR : 835.669 delta(WSSR)/WSSR : 0delta(WSSR) : 0 limit for stopping : 1e05lambda : 1.4634

initial set of free parameter values

m = 1c = 1/

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Iteration 1WSSR : 37.2229 delta(WSSR)/WSSR : 21.4504delta(WSSR) : 798.446 limit for stopping : 1e05lambda : 0.14634

resultant parameter values

m = 4.82373c = 4.76338/



m = 0.671102c = 13.3427/



m = 0.361653c = 13.9148/

Iteration 4WSSR : 0.00507835 delta(WSSR)/WSSR : 1.21954e05delta(WSSR) : 6.19328e08 limit for stopping : 1e05lambda : 0.00014634


45


m = 0.361441c = 13.9152**/

Iteration 5WSSR : 0.00507835 delta(WSSR)/WSSR : 6.83184e16delta(WSSR) : 3.46945e18 limit for stopping : 1e05lambda : 0.0014634


m = 0.361441c = 13.9152

After 5 iterations the fit converged.final sum of squares of residuals : 0.00507835rel. change during last iteration : 6.83184e16

degrees of freedom (ndf) : 4rms of residuals (stdfit) = sqrt(WSSR/ndf) : 0.0356313variance of residuals (reduced chisquare) = WSSR/ndf : 0.00126959

Final set of parameters Asymptotic Standard Error======================= ==========================

m = 0.361441 +/ 0.03095 (8.563%) (here this is the coefficient)c = 13.9152 +/ 0.05608 (0.403%)

correlation matrix of the fit parameters:

m cm 1.000c 0.966 1.000gnuplot> replot y(x) then it will plot the line over the graph.if the plot is not good ......the percentage of error is too much then put the # mark infront of the stardetails.like...below then you can see the percentage of error will be less now.

46


1 14.324 0.011 csa104v01.fits 1.14161 14.337 0.011 csa104v02.fits 1.1505#1 15.183 0.014 csa104v03.fits 1.54061 14.508 0.011 csa104v04.fits 1.76191 14.637 0.011 csa104v05.fits 1.90121 14.728 0.013 csa104v06.fits 2.15441 14.752 0.012 csa104v07.fits 2.3898

*******************************************************************************Fri Aug 4 15:50:26 2006FIT: data read from "magv1" u 5:2 #datapoints = 6 residuals are weighted equally (unit weight)

function used for fitting: y(x)fitted parameters initialized with current variable values

Iteration 0WSSR : 0.07522 delta(WSSR)/WSSR : 0delta(WSSR) : 0 limit for stopping : 1e05lambda : 1.4634

initial set of free parameter values

m = 0.26786c = 14.1777 190,01 After 4 iterations the fit converged.final sum of squares of residuals : 0.00507835rel. change during last iteration : 6.80346e09

degrees of freedom (ndf) : 4rms of residuals (stdfit) = sqrt(WSSR/ndf) : 0.0356313variance of residuals (reduced chisquare) = WSSR/ndf : 0.00126959

Final set of parameters Asymptotic Standard Error======================= ==========================

m = 0.361441 +/ 0.03095 (8.563%)c = 13.9152 +/ 0.05608 (0.403%)

correlation matrix of the fit parameters: m c

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m 1.000c 0.966 1.000Also it will create an log file to save this information.onitself as fit.log file.awk '{print($50.36*$7)}' obsmag

11 Spectroscopy reduction Hints:1.First do everything with the specred....means u cant do apall with onedspec command.....so enter in tospecred then to onedspec.2.you cant do everything with specred .because ,while calibrating u have to mention the place (filenamewhere it is located ..like onestds$spec50cal )it is available only in the onedspec so onedspec isimportant....unless we are keeping the file in our own place)

For deleting the .imh file >imdel <filename.imh>

Requirements:1.object167 l2.Standard two(Oke 1990)1340 l3.comparision(FeAr)4.flat (Halogen lamp)5.bias*Grism with respct to wavelength coverage.

Part1.basic Steps changing the name into .fits file.>pc120001 >epar renamefiles = pc* list of files to be renamednewname = fits new file name or field name(field = extn) field to be modified (all|ldir|root|extn)(mode = ql):go>imhead pc120047.fitspc120047.fits[500,3500][ushort]: NGC 4216cc> emv pc120047.fits n42162.fitscl> noao artdata. digiphot. nobsolete. onedspec. astcat. focas. nproto. rv.

48


astrometry. imred. observatory surfphot. astutil. mtlocal. obsutil. twodspec. no> im argus. crutil. echelle. iids. kpnocoude. specred. bias. ctioslit. generic. irred. kpnoslit. vtel. ccdred. dtoi. hydra. irs. quadred. im> cc badpiximage ccdmask flatcombine mkskyflat ccdgroups ccdproc mkfringecor setinstrument ccdhedit ccdtest mkillumcor zerocombine ccdinstrument combine mkillumflat ccdlist darkcombine mkskycor cc> specred aidpars@ apresize dispcor response skysub apall apscatter dofibers sapertures skytweak apdefault@ apsum dopcor sarith slist apedit aptrace doslit scombine specplot apfind autoidentify fitprofs scopy specshift apfit background identify sensfunc splot apflatten bplot illumination setairmass standard apmask calibrate msresp1d setjd telluric apnormalize continuum refspectra sfit aprecenter deredden reidentify sflip

sp> ls(go into the respective file)

sp> epar imcombine

PACKAGE = immatch TASK = imcombine (the changable parameters are): input = bias*.fits List of images to combineoutput = mbias.fits List of output images(combine= median) Type of combine operation

49


(reject = avsigclip) Type of rejection(rdnoise= 4.8) ccdclip: CCD readout noise (electrons)(gain = 1.22) ccdclip: CCD gain (electrons/DN):goJun 13 11:41: IMCOMBINE combine = median, scale = none, zero = none, weight = none reject = avsigclip, mclip = yes, nkeep = 1 lsigma = 3., hsigma = 3. blank = 0. Images Offsets bias1.fits 0 0 bias2.fits 0 0 bias3.fits 0 0 bias4.fits 0 0 bias5.fits 0 0 bias6.fits 0 0 bias7.fits 0 0

Output image = mbias.fits, ncombine = 7cc> display mbias.fitsframe to be written into (1:16) (1): z1=273.2498 z2=299.

sp>imstat mbias.fits[3:480,243:3200] means x,y limitation# IMAGE NPIX MEAN STDDEV MIN MAX mbias.fits[3:480,243:3200] 1413924 349.2 49.55 259. 834.

sp> imarith g19b2b2.fits 349.2 bg19b2b2.fits

(just like do for all images....exept fear)

sp> imstat bhal?.fits# IMAGE NPIX MEAN STDDEV MIN MAX bhal1.fits 1750000 8221. 9342. 349.2 52146. bhal2.fits 1750000 8226. 9349. 349.2 52172. bhal3.fits 1750000 8238. 9363. 349.2 52271. bhal4.fits 1750000 8231. 9356. 349.2 52320. bhal5.fits 1750000 8247. 9373. 349.2 52336.

50


(then take mean of mean)....here ..the mean is 8233sp>imarith bhal1fits / 8233 nbhal1.fits (like that do for all)sp> epar imcombine

PACKAGE = immatch TASK = imcombine input = nbhal*.fits List of images to combineoutput = fnbhal.fits List of output images(combine= median) Type of combine operation(reject = avsigclip) Type of rejection:goJun 14 11:28: IMCOMBINE combine = median, scale = none, zero = none, weight = none reject = avsigclip, mclip = yes, nkeep = 1 lsigma = 3., hsigma = 3. blank = 0. Images nbhal1.fits nbhal2.fits nbhal3.fits nbhal4.fits nbhal5.fits

Output image = fnbhal.fits, ncombine = 5sp> epar responsecalibrat= fnbhal.fits Longslit calibration imagesnormaliz= fnbhal.fits Normalization spectrum imagesresponse= rfnbhal.fits Response function images(functio= spline3) Fitting function(order = 3) Order of fitting function:goFit the normalization spectrum for fnbhal.fits interactively (yes):nosp>imarith bm1061.fits / rfnbhal.fits fbm1061.fitssp>onedspec

51


Part2.Wavelength Calibartionsp>epar apall

(better do not give the output name...it will take automatically with extension of .ms.imh)

# EXTRACTION PARAMETERS

(backgro= median) Background to subtractearlier it was fit but for median works fine.(skybox = 1) Box car smoothing length for sky(weights= variance) Extraction weights (none|variance)(pfit = fit2d) Profile fitting type (fit1d|fit2d)(clean = yes) Detect and replace bad pixels?(saturat= 63000.) Saturation level(readnoi= 4.87) Read out noise sigma (photons)(gain = 1.22) Photon gain (photons/data number)(lsigma = 4.) Lower rejection threshold(usigma = 4.) Upper rejection threshold(nsubaps= 1) Number of subapertures per aperture(mode = ql)mbias.fits

:go Recenter apertures for fbm1061? (yes): Resize apertures for fbm1061? (yes): Edit apertures for fbm1061? (yes): (then the graph will appear)

then set the aperture giving lower and upper limit .By pressing "l" lower limit.By pressing "u" upper limit.

Then for background subtraction....press "b"Then "f ":sample 25:20,20:25 (or).......in wavelengh calibartion for sky substraction just to mark the limits...instead of typing :sample.....type simly by the keys..thatusing the s & t where s—for marking level..

52


where t –for unmarking..Then..." f "change the order to 3 by:order 3(now RMS value will be reduced)" q "yes,yes,yes,...

Then the fitted curve will appear...delete the points (by "d")which is apart from the line.and try toreduce reduce the RMS value.Then for quit.." q "write the apertures to database:yes,yes,...Then the spectrum of object will be shown.( for a group of images also we can do at one time...one by one...in the input list of images by giving*.fits)

Do this apall for the standard star also...

on>splot nobject.fitson>splot nobject_spec.imhon>apall fear1 out=fear_spec refer=nobject.fits recen trac back interac(so now fear_spec.imh file has been created)(here also by group we can create spectra by giving *.fits).

sp>epar identifyimages = fear_spec Images containing features to be identified(section= middle line) Section to apply to two dimensional images(databas= database) Database in which to record feature data(coordli= /home/chrisphin/bin/fear.dat) User coordinate list(functio= legendre) Coordinate function:go(then the graph of comparision fear will open)Then using *commands and comparing the paper ....plot the wavelength on it.minimum should be 12.

*Note:to extend on x axis shift+x

53


To extend on Y axisshift+yfo markingmto come back and do againrfjfqThen the fitted curve will appear...delete the points (by "d")which is apart fromthe line.and try to reduce reduce the RMS value.ljf (here f=j ..so use f itself)q(ffitting, jrisidual plot,l=longitudinal plot, lit will plot remaining wavelengths on its own)(" i " will delete the all lines which is marked already)then in xgterm....writing the data structures in database?yes

This identification only one time is enough which can be used for all.Just hedit and add to all this asreference.

sp> hedit nobject_1_spec.imh field=REFSPEC1 value=fear_spec.imh hedit fm1061spec.imh field=REFSPEC1 value=fearspec.imhadd fm1061spec.imh,REFSPEC1 = fearspec.imhupdate fm1061spec.imh ? (yes): bm1061_spec.imh updated

sp> epar dispcorinput = nobject1_spec.imh List of input spectraoutput = wobject1_spec.imh List of output spectra(lineari= yes) Linearize (interpolate) spectra?(databas= database) Dispersion solution database(ignorea= yes) Ignore apertures?(incase if u have selected different apertures)

:go

TTFbn1569_3.ms.imh: REFSPEC1 = 'TFbcp_2.ms.imh 1.'Dn1569_3.ms.imh: ap = 1, w1 = 2524.67, w2 = 7955.183, dw = 1.552019, nw = 3500After dispersion correction make it all subexposures as one using the command “ sarith “ one by one

For atmospheric line correction s type: better to do this after flux calibration (in case if we are interested in flux calibration also.)First identify the differnce between actual to the observed atmospheric lines then using

>epar specshiftPACKAGE = specred

54


TASK = specshift

spectra = List of spectrashift = 0. Shift to add to dispersion coordinates(apertur= ) List of apertures to shift(verbose= no) Print verbose information?(mode = ql)

For doppler corection:>epar dop

PACKAGE = specred TASK = dopcor

input = List of input spectraoutput = List of output spectraredshift= Redshift or velocity (Km/s)(isveloc= no) Is the redshift parameter a velocity?(add = no) Add to previous dispersion correction?(dispers= yes) Apply dispersion correction?(flux = no) Apply flux correction?(factor = 3.) Flux correction factor (power of 1+z)(apertur= ) List of apertures to correct(verbose= no) Print corrections performed?(mode = ql):go

Part3.Flux Calibiration

Before starting the Flux calibartaion....set airmass and set the observatory parameters.

sp> epar standard

Here the input is dispersion corrected standard star.{ in this... the symbol )_.observatory meant that it will take the information from main}

PACKAGE = onedspec TASK = standard

55


input = Dstd_2.ms.imh Input image file root nameoutput = std Output flux file (used by SENSFUNC)(samesta= yes) Same star in all apertures?(beam_sw= no) Beam switch spectra?(apertur= ) Aperture selection list(bandwid= INDEF) Bandpass widths(bandsep= INDEF) Bandpass separation(fnuzero= 3.6800000000000E20) Absolute flux zero point(extinct= /home/observer/chris/bin/spec_ext.dat) Extinction file(caldir = onedstds$/spec50cal/) Directory containing calibration data(observa= )_.observatory) Observatory for data(interac= yes) Graphic interaction to define new bandpasses(graphic= stdgraph) Graphics output device(cursor = ) Graphics cursor inputstar_nam= feige34 Star name in calibration listairmass = Airmassexptime = Exposure time (seconds)mag = Magnitude of starmagband = Magnitude typeteff = Effective temperature or spectral typeanswer = no (no|yes|NO|YES|NO!|YES!)(mode = ql)

:go

Dstd_2.ms.imh[*,1,1](1): Star name in calibration list (g191b2b): Dstd_2.ms.imh[1]: Edit bandpasses? (no|yes|NO|YES|NO!|YES!) (no):

Now you can see the file std has been created with the details of [Dstd_2.ms.imh] 1 3401 600.00 3.602 349.000 3749.000 G19B2B 3200.00 4.6598E13 50.000 3417. 3250.00 4.3944E13 50.000 2187.5 3300.00 4.4222E13 50.000 1189.7 3350.00 4.2912E13 50.000 885.67 3400.00 4.0899E13 50.000 786.2 3450.00 3.8639E13 50.000 778.63 3500.00 3.6185E13 50.000 993.41 3550.00 3.5173E13 50.000 512.38

56


3600.00 3.3271E13 50.000 387.07 3650.00 3.1775E13 50.000 152.9 3700.00 3.0357E13 50.000 51.126

hint:Even after sploting ...if the graph doesnt come press “a” two times.

Then the scale will change to bring the picture.

By typing the below you can get the location where the respective standard star location is...

for getting standard ....observatory is needed also airmass also location of the caldirectory withinIRAF has to be specified..needed..hence for setting these...follow the below...

sp> help onedstd

Standard stars in onedstds$spec50cal/ (3200A 10200A)

bd284211 eg247 feige34 g191b2b hz44 eg139 eg71 feige66 gd140 pg0823546 eg158 feige110 feige67 hilt600 wolf1346

sp> epar sens

PACKAGE = onedspec TASK = sensfunc

standard= std Input standard star data file (from STANDARD)sensitiv= sens Output root sensitivity function imagename(apertur= ) Aperture selection list(ignorea= yes) Ignore apertures and make one sensitivity function?(logfile= logfile) Output log for statistics information(extinct= /home/observer/chris/bin/spec_ext.dat) Extinction file(newexti= extinct.dat) Output revised extinction file

57


(observa= )_.observatory) Observatory of data(functio= spline3) Fitting function(order = 6) Order of fit(interac= yes) Determine sensitivity function interactively?(graphs = sr) Graphs per frame(marks = plus cross box) Data mark types (marks deleted added)(colors = 2 1 3 4) Colors (lines marks deleted added)(cursor = ) Graphics cursor input(device = stdgraph) Graphics output deviceanswer = yes (no|yes|NO|YES)(mode = ql):go

Fit aperture 1 interactively? (no|yes|NO|YES) (no|yes|NO|YES) (yes):

Then the graph will open.

Change the order to 9.:ord 9then “ r “ replot“ d “delete the deviated points in the below figure.“ f “ fit “ r “ replotNow you can see RMS value has been reduced.After finishing “ q “quit

sp> epar cali

Here the input is dispersion corrected object.

PACKAGE = onedspec TASK = calibrate

input = Dn1569_1.ms.imh Input spectra to calibrateoutput = Fn1569_1.ms.imh Output calibrated spectra(extinct= yes) Apply extinction correction?(flux = yes) Apply flux calibration?(extinct= /home/observer/chris/bin/spec_ext.dat) Extinction file(observa= )_.observatory) Observatory of observation

58


(ignorea= yes) Ignore aperture numbers in flux calibration?(sensiti= sens) Image root name for sensitivity spectra(fnu = no) Create spectra having units of FNU?airmass = Airmassexptime = Exposure time (seconds)(mode = ql)

:go

Fn1569_1.ms.imh: NGC1569 Cn1569_1.imh: NGC1569 Extinction correction applied Flux calibration appliedThe above warning because of trimmming may be..

Then sploting the final wavelength and flux calibrated spectrum will appear.

Some more hints on spectroscopy reduction:

1.Removing unwanted lined by the bad pixel:After splotting find out the line ...and place the cursor then press the “ x “ on both the end of the raythen press “ r “ ...then it will be removed.2.EQW:For finding the equalent width press “ e “ on both the ends.3. “ f “ for finding the apertureswhere “ d” for delete the apeture....so if any cosmic ray prsent and aperture goes for that ...then pres ffor finding apeture then dlete the another unwanted aperture.

while doing apall if 2 or 3 features wanted to extract at one time then use shift + it will take to anotherpeak...then extract..4.While epar identification better to use spline 3....and always order 3 is nice. “ j “ fo residual plot.After getting spectrum...There are 4 atmospheric lines....2 are in absorbtion...whar e the 7605 is visible clearly.....then 6870..then in epar splot select the band number as 2.then splotting you will get again 2 lines.6300,6364.

59


in the splot graphby typing k,k two times u can get the value of fwhm....and others.

for saving the graph:.snap epsflTo get the list of help commands press ? from graphical window.then it will give the list in xgterm window like .................

1. INTERACTIVE CURVE FITTING CURSOR OPTIONS

? Print optionsa Add point to constrain fitc Print the coordinates and fit of point nearest the cursord Delete data point nearest the cursorf Fit the data and redraw or overplotg Redefine graph keys. Any of the following data types may be along either axis. x Independent variable y Dependent variable f Fitted value r Residual (y f) d Ratio (y / f) n Nonlinear part of yhl Graph keys. Defaults are h=(x,y), i=(y,x), j=(x,r), k=(x,d), l=(x,n)o Overplot the next graphq Exit the interactive curve fitting. Carriage return will also exit.r Redraw graphs Set sample range with the cursort Initialize the sample range to all pointsv Change the weight of the point nearest the cursoru Undelete the deleted point nearest the cursorw Set the graph window. For help type 'w' followed by '?'.x Change the x value of the point nearest the cursory Change the y value of the point nearest the cursorz Delete sample region nearest cursorI Interrupt task immediately

2. INTERACTIVE CURVE FITTING COLON COMMANDS

The parameters are listed or set with the following commands which may beabbreviated. To list the value of a parameter type the command alone.

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:show [file] Show the values of all the parameters:vshow [file] Show the values of all the parameters verbosely:xyshow [file] Show the x, y, y fit, and weight data values:evaluate <value> Print the fit at the specified value:errors [file] Print the errors of the fit (default STDOUT):function [value] Fitting function (chebyshev, legendre, spline3, spline1):grow [value] Rejection growing radius:naverage [value] Sample averaging or medianing window:order [value] Fitting function order:low_reject [value] Low rejection threshold:high_reject [value] High rejection threshold:niterate [value] Number of rejection iterations:sample [value] Sample ranges:markrej [value] Mark rejected points?

Additional commands are available for setting graph formats and manipulatingthe graphics. Use the following commands for help.

:/help Print help for graph formatting option:.help Print help for general graphics options

3. INTERACTIVE CURVE FITTING GRAPH KEYS

The graph keys are h, i, j, k, and l. The graph keys may be redefined toput any combination of axes types along either graph axis with the 'g' key.To define a graph key select the desired key to redefine and then specifythe axes types for the horizontal and vertical axes by a pair of commaseparated types from the following:

d Ratio (y / f)f Fitted valuesr Residuals of fit (y f)n Nonlinear part of data (linear component of fit subtracted)x Indepedent variabley Dependent variable (data being fit)

? This display r Redraw the current window/ Cycle thru short help on stat line s Smooth (boxcar)a Autoexpand between cursors t Fit continuum(*)

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b Toggle base plot level to 0.0 u Adjust coordinate scale(*)c Clear and redraw full spectrum v Velocity scale (toggle)d Deblend lines using profile models w Window the graphe Equiv. width, integ flux, center x Connects 2 cursor positionsf Arithmetic functions: log, sqrt... y Plot std star flux from calib fileg Get new image and plot z Expand x range by factor of 2h Equivalent widths(*) ) Go to next spectrum in imagei Write current image as new image ( Go to previous spectrum in imagej Fudge a point to Ycursor value # Select new line/aperturek Profile fit to single line(*) % Select new bandl Convert to Flambda $ Toggle wavelength/pixel scalem Mean, RMS, snr in marked region Subtract deblended fitn Convert to Fnu , Down slide spectrumo Toggle overplot of following plot . Up slide spectrump Convert to wavelength scale I Interrupt task immediatelyq Quit and exit <space> Cursor position and flux

(*) For 'h' key: Measure equivalent widths a Left side for width at 1/2 flux l Left side for continuum = 1 b Right side for width at 1/2 flux r Right side for continuum = 1 c Both sides for width at 1/2 flux k Both sides for continuum = 1

(*) For 'k' key: Second key may be used to select profile type g Gaussian, l Lorentzian, v Voigt, all others Gaussiank

(*) For 't' key: Fit the continuum with ICFIT and apply to spectrum / = normalize by the continuum fit = subtract the continuum fit (residuals) f = replace spectrum by the continuum fit c = clean spectrum of rejected points n = do the fitting but leave the spectrum unchanged q = quit without fitting or modifying spectrum

(*) For 'u' key: Adjust the coordinate scale by marking features d = apply doppler correction to bring marked feature to specified coord. l = set linear (in wavelength) coordinates based on two marked features z = apply zero point shift to bring marked feature to specified coordinate

The colon commands do not allow abbreviations.

:# <comment> Add comment to log file

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:dispaxis <val> Change summing parameter for 2D images:log Enable logging to save_file:nolog Disable logging to save_file :nsum <val> Change summing parameter for 2D images:show Show full output of deblending and equiv. width measurments:units <value> Change coordinate units (see below)

:label <label> <format> Add label at cursor position:mabove <label> <format> Add tick mark and label above spectrum:mbelow <label> <format> Add tick mark and label below spectrum The label must be quoted if it contains blanks. A label beginning with % (i.e. %.2f) is treated as a format for the x cursor position. The optional format is a gtext string (see help on "cursors"). The labels are not remembered between redraws.

:auto [yes|no] Enable/disable autodraw option:zero [yes|no] Enable/disable zero baseline option:xydraw [yes|no] Enable/disable xydraw option:hist [yes|no] Enable/disable histogram line type option:nosysid [yes|no] Enable/disable system ID option:wreset [yes|no] Enable/disable window reset for new spectra option:flip [yes|no] Enable/disable dispersion coordinate flip:overplot [yes|no] Enable/disable permanent overplot mode

:/help Get help on GTOOLS options:.help Get help on cursor mode options

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12.LATEX Introduction While doing latex to ps do it one folder so the all sub created file will be within the folder itself. >vi hct_obsp_new.tex> latex hct_obsp_new.texThis is TeX, Version 3.14159 (Web2C 7.4.5) Output written on hct_obsp_new.dvi (5 pages, 10872 bytes).Transcript written on hct_obsp_new.log.[chrisphin@aries25 ~/hct_form]$ dvips o hct_obsp_new.ps hct_obsp_new.dviThis is dvips(k) 5.92b Copyright 2002 Radical Eye Software (www.radicaleye.com)' TeX output 2006.11.01:1541' > hct_obsp_new.ps

> gv hct_obsp_new.ps>ps2pdf hct_obsp_new.ps hct_obsp_new.pdf>xpdf hct_obsp_new.pdf

for a short cut.......you can open a vi editer and put all the commands which has to be executed andthen execute that file which will do all the work by one stroke.>vi llatex hct_obsp_new.texdvips o hct_obsp_new.ps hct_obsp_new.dvigv hct_obsp_new.ps:wq>chmod 777 l>./l

General format example:\documentstyle[a4,12pt,psfig]{article}\textheight 18.0cm\textwidth 16.0cm\topmargin 1.0cm\begin{document}\begin{center}{\Large \bf Photometric and Spectrophotometric studies on WolfRayet Galaxies }\\\vspace{1.0cm}\bf Chrisphin.K, B.B.Sanwal,D.K.sahu, M.Singh\\\small \bf Aryabhatta Research Institute ofObservational Sciences(ARIES)\\Manora Peak,Nainital. \\

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\vspace{0.5cm}{\small \it email: [email protected]}\end{center}\bigskip\begin{abstract}

\end{abstract}\end{document}Latex.....commmand.....\item ...........for point..s 1,2,3....like that.if infront of the letter if we put % symbol then it wont come.\sectionfor subsection\section*then it wont put any number...like 2.1,2.2,...like that.

Some commmands quite often used by astronomers in Latex:

HeII 4686$ \AA $He II 4686 A° 2k$\times$2k2K x 2KH$\alpha$ \& H$\alpha$ H

In escape mode...5dddeleting 5lines.like that any number of lines..uundo5yy5 lines copyingppaste.for cutting use the same command for deletingddredoctrl+r

above all is in escape mode.Type <return> to proceed, S to scroll future error messages,R to run without stopping, Q to run quietly,I to insert something,H for help, X to quit.? X\begin{tabular}{|p{.35in}|p{.9in}|p{1.1in}|p{1.1in}|p{0.6in}|p{0.5in}|p{0.3in}|}\hlineSl.No.&Objects Name& RA (hh mm ss) at J2000.0. & Dec (dd mm ss) at J2000.0.& $V$/int.$V$ mag & Filter & Min. S/N\\

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\hline & & & & & &\\ \hline & & & & & &\\ \hline & & & & & &\\ \hline & & & & & &\\ \hline\end{tabular}

\newpage\vskip 2cmif you want to jump to 30 th line in vi editor..then type:30and all the commnad s is possible to execute from..the same terminal..by typing..:!latex <filename>:!dvips o filename.ps filename.dvi

Finding the SFR the expression is:

SFR$_{H\alpha} (M_\odot year^{1})= 7.9 \times 10^{42} L_{H\alpha}$

\hspace*{0.1in} –while beginnning sentence giving space.

for inserting the fgure:

\usepackage{graphicx}\begin{document}\label{firstpage}\begin{figure}\vbox{\includegraphics[height=12cm,width=12cm,angle=90]{/home/chrisphin/spectrum/final_figure/2_n1569.ps}\includegraphics[height=12cm,width=12cm,angle=90]{/home/chrisphin/spectrum/final_figure/2_m33.ps}}\caption{Nuclear Spectrum of NGC 1569 and NGC Mrk 33 respectively}\end{figure}

angle if needed only.

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13.Ellipse Fittingchrisphin > cl NOAO PCIRAF Revision 2.12.2EXPORT Sun Jan 25 16:09:03 MST 2004 This is the EXPORT version of PCIRAF V2.12 supporting most PC systems.

Welcome to IRAF. To list the available commands, type ? or ??. To get detailed information about a command, type `help command'. To run a command or load a package, type its name. Type `bye' to exit a package, or `logout' to get out of the CL. Type `news' to find out what is new in the version of the system you are using. The following commands or packages are currently defined:

dataio. language. obsolete. softools. tables. dbms. lists. plot. stsdas. utilities. images. noao. proto. system. cl> stsdas

++ | Space Telescope Science Data Analysis System | | STSDAS Version 3.3, November 11, 2004 | | | | Space Telescope Science Institute, Baltimore, Maryland | | Copyright (C) 2003 Association of Universities for | | Research in Astronomy, Inc.(AURA) | | See stsdas$copyright.stsdas for terms of use. | | For help, send email to [email protected] | | | ++ analysis. describe fitsio. hst_calib. problems toolbox. contrib. examples graphics. playpen. sobsolete. st> an dither. fourier. isophote. restore. fitting. gasp. nebular. statistics. an> is bmodel geompar@ isomap magpar@ controlpar@ isoexam isopall samplepar@ ellipse isoimap isoplot

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is> epar ellipsePACKAGE = isophote TASK = ellipse

input = n4449B.fits input image name cleaned galaxy imageoutput = b output table name(dqf = .c1h) data quality file name or extension (inellip= ) table with input ellipses for nofit mode(geompar= ) geometric parameters (pset)(control= ) algorithm control parameters (pset)(samplep= ) sampling control parameters (pset)(magpar = ) magnitude scale parameters (pset)(interac= no) interactive ?(device = red) graphics output device(icomman= ) image cursor(gcomman= ) graphics cursor(masksz = 5) pixel square mask size (`m' cursor key)(region = no) region masking mode ?(memory = yes) memoryintensive (versus diskintensive) ?(verbose= yes) list summary at STDOUT ?(mode = al) (bring the cursor in geompar and press :e then this will come fill the respective.normally the geompar and control is the important.)

PACKAGE = isophote TASK = geompar

(x0 = INDEF) initial isophote center X(y0 = INDEF) initial isophote center Y(ellip0 = 0.2) initial ellipticity(pa0 = 20.) initial position angle (degrees)(sma0 = 10.) initial semimajor axis lenght(minsma = 0.) minimum semimajor axis lenght(maxsma = INDEF) maximum semimajor axis lenght(step = 0.1) sma step between successive ellipses(linear = no) linear sma step ?

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(maxrit = INDEF) maximum sma lenght for iterative mode(recente= yes) allows finding routine to recenter x0y0 ?(xylearn= yes) updates pset with new x0y0 ?(physica= yes) physical coordinate system ?(mode = al)

:qthen press :e by placing the cursor on control Image Reduction and Analysis FacilityPACKAGE = isophote TASK = controlpar

(conver = 0.05) convergency criterion (maximum harmonic amplitud(minit = 10) minimun no. of iterations at each sma(maxit = 50) maximun no. of iterations at each sma(hcenter= no) hold center fixed ?(hellip = no) hold ellipticity fixed ?(hpa = no) hold position angle fixed ?(wander = INDEF) maximum wander in successive isophote centers(maxgerr= 0.5) maximum acceptable gradient relative error(olthres= 1.) object locator's ksigma threshold(soft = no) soft stop ?(mode = al)

:q

PACKAGE = isophote TASK = samplepar

(integrm= bilinear) area integration mode(usclip = 3.) sigmaclip criterion for upper deviant points(lsclip = 3.) sigmaclip criterion for lower deviant points(nclip = 0) number of sigmaclip iterations(fflag = 0.5) acceptable fraction of flagged data points (sdevice= none) graphics device for ploting intensity samples(tsample= none) tables with intensity samples(absangl= yes) sample angles refer to image coord. system ? (harmoni= none) optional harmonic numbers to fit(mode = al)

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:q

PACKAGE = isophote TASK = magpar

(mag0 = 0.) magnitude of reference source(refer = 1.) intensity of reference source (zerolev= 0.) intensity of zero (bias) level (mode = al):qthen:goRunning object locator... Done.Can not find object. Please, enter initialguess for starting isophote center:X0: 485Y0: 545#

# Semi Isophote Ellipticity Position Grad. Data Flag Iter. Stop# major mean Angle rel. code# axis intensity error#(pixel) (degree)# 10.00 852.25(322.98) 0.200(INDEF) 20.00(INDEF) INDEF 56 0 2 4 11.00 902.56(479.69) 0.200(INDEF) 20.00(INDEF) INDEF 62 0 1 4 9.09 812.00(227.45) 0.200(INDEF) 20.00(INDEF) INDEF 51 0 2 4 8.26 787.88(183.00) 0.200(INDEF) 20.00(INDEF) INDEF 46 0 1 4 7.51 774.51(167.34) 0.200(INDEF) 20.00(INDEF) INDEF 42 0 1 4 6.83 773.30(158.86) 0.200(INDEF) 20.00(INDEF) INDEF 38 0 1 4 6.21 775.17(152.67) 0.200(INDEF) 20.00(INDEF) 19.53 35 0 1 4 5.64 785.31(142.66) 0.200(INDEF) 20.00(INDEF) 3.560 32 0 1 4 5.13 799.19(133.24) 0.200(INDEF) 20.00(INDEF) 2.546 29 0 1 4 4.67 814.31(122.95) 0.200(INDEF) 20.00(INDEF) 2.284 26 0 1 4 4.24 825.31(112.12) 0.200(INDEF) 20.00(INDEF) 3.023 24 0 1 4 3.86 836.47(102.91) 0.200(INDEF) 20.00(INDEF) 2.839 22 0 1 4 3.50 845.04( 95.28) 0.200(INDEF) 20.00(INDEF) 3.571 20 0 1 4 3.19 852.90( 88.52) 0.200(INDEF) 20.00(INDEF) 3.795 18 0 1 4 2.90 855.50( 83.38) 0.200(INDEF) 20.00(INDEF) 11.16 17 0 1 4 2.63 863.26( 77.85) 0.200(INDEF) 20.00(INDEF) 3.675 15 0 1 4 2.39 865.60( 73.17) 0.200(INDEF) 20.00(INDEF) INDEF 14 0 1 4 2.18 871.25( 68.40) 0.200(INDEF) 20.00(INDEF) 4.825 13 0 1 4 1.98 872.41( 64.20) 0.200(INDEF) 20.00(INDEF) 3.854 13 0 1 4 1.80 874.40( 59.60) 0.200(INDEF) 20.00(INDEF) 12.15 13 0 1 4

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1.64 876.17( 55.01) 0.200(INDEF) 20.00(INDEF) 12.71 13 0 1 4 1.49 877.63( 50.27) 0.200(INDEF) 20.00(INDEF) 14.17 13 0 1 4 1.35 879.08( 46.06) 0.200(INDEF) 20.00(INDEF) 13.07 13 0 1 4 1.23 880.09( 42.18) 0.200(INDEF) 20.00(INDEF) 17.21 13 0 1 4 1.12 880.76( 38.58) 0.200(INDEF) 20.00(INDEF) 23.35 13 0 1 4 1.02 881.15( 34.98) 0.200(INDEF) 20.00(INDEF) 37.93 13 0 1 4 0.92 881.38( 31.62) 0.200(INDEF) 20.00(INDEF) 56.84 13 0 1 4 0.84 881.55( 28.60) 0.200(INDEF) 20.00(INDEF) 68.24 13 0 1 4 0.76 881.68( 25.89) 0.200(INDEF) 20.00(INDEF) 82.65 13 0 1 4 0.69 881.77( 23.45) 0.200(INDEF) 20.00(INDEF) 104.1 13 0 1 4 0.63 881.84( 21.25) 0.200(INDEF) 20.00(INDEF) 134.5 13 0 1 4 0.57 881.88( 19.26) 0.200(INDEF) 20.00(INDEF) 186.7 13 0 1 4 0.52 881.90( 17.47) 0.200(INDEF) 20.00(INDEF) 287.5 13 0 1 4 0.00 881.45 0.01 CPU seconds. 0.00 minutes elapsed.

>ls

now if you see list b.tab file has been created.to view that file type >tprint b.tab

>epar isoexamPACKAGE = isophote TASK = isoexam

table = b.tab isophote table(dqf = .c1h) data quality file name or extension (device = red) graphics output device(icomman= ) image cursor(gcomman= ) graphics cursor(mode = al)

:q

>epar isoimapPACKAGE = isophote TASK = isoimap

image = n4449B.fits input imagetable = b.tab input table

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(fulltab= yes) use full range of `SMA' from table ?(minsma = 1.) minimum semimajor axis(maxsma = 1.) maximum semimajor axis(nlevels= 3) number of levels(color = r) overlay color(frame = 1) image display frame(mode = al):qis> epar isomap

PACKAGE = isophote TASK = isomap

image = n4449B.fits input imagetable = b.tab input tablefloor = minimum contouring levelceiling = maximum contouring level(nlevels= 3) number of levels(device = stdgraph) graphics device(mode = al):q

>epar isoplot

PACKAGE = isophote TASK = isoplot

input = b.tab input tablexaxis = RSMA x axisyaxis = MAG y axis(device = stdgraph) output graphics device(mode = al)

:go(will give the plot for mag vs SMA *1/4)

>epar isopallinput = b.tab input tablexaxis = RSMA x axis

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(device = stdgraph) output graphics device(mode = al)

:go

(will give the plot for all)

is>ttoolstt>tprint

tt> ? gtedit tabkey tcreate tiimage tprint tstat gtpar@ tabpar tdelete tinfo tproduct ttranspose imtab taextract tdiffer tintegrate tproject tunits keypar tainsert tdump titable tquery tupar keyselect tcalc tedit tjoin tread tximage keytab tchcol texpand tlcol trebin txtable parkey tcheck thedit tlinear tscopy partab tchsize thistogram tmatch tselect tabim tcopy thselect tmerge tsort

tt> tcalcInput table: b.tabOutput column name: magbArithmetic expression: 2.5*log10(INTENS)

(then in the output table b.tab one more column has fomed with magb)like that find out for v&r

tt> tprojInput tables (b): vOutput tables (b1): v1Column names (sma,magb): sma,magv

this will give the output table with only two colum as sma and magv from original table.tt> tmergelist of tables: b1,v1,r1name of output table: bvr

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merge or append? (merge|append) (merge):

This will give the output as with the common one (ie..sma)and the individual magnitudes.

tt> tcalcInput table (r.tab): bvrOutput column name (magr): bvArithmetic expression (2.5*log10(INTENS)): magbmagv

then the output is.....

# row SMA magb magv magr bv# pixel

1 10.00 7.326419 8.350383 8.977684 1.023964 2 11.00 7.388693 8.402966 9.018461 1.014274 3 12.10 7.452424 8.45775 9.061924 1.005327

tt> tcalcInput table (bvr): Output column name (bv): vrArithmetic expression (magbmagv): magvmagrtt> tprint bvr# row SMA magb magv magr bv # pixel

1 10.00 7.326419 8.350383 8.977684 1.023964 2 11.00 7.388693 8.402966 9.018461 1.014274 vr#

1 0.6273012 2 0.6154947

for making a model using the table parameterstt> epar bmodel

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PACKAGE = isophote TASK = bmodel

table = b.tab isophote tableoutput = bm.fits output (model) image(parent = b.fits) parent image(fulltab= yes) use full range of `SMA' from table ?(minsma = 1.) minimum modelling SMA(maxsma = 1.) maximum modelling SMA(backgr = 0.) background value(interp = spline) interpolation algorithm(highar = no) add higher harmonics ?(verbose= no) print info ?(mode = ql)

:go

then the model image will appear.

tt> imarith b.fits bm.fits subb.fits

(substracting from parent image to model image)

# Table bvr.tab Tue 14:13:23 25Jul2006

# row SMA magb magv magr bv vr# pixel

1 10.00 7.326419 8.350383 8.977684 1.023964 0.6273012 2 11.00 7.388693 8.402966 9.018461 1.014274 0.6154947 3 12.10 7.452424 8.45775 9.061924 1.005327 0.6041737 4 13.31 7.509982 8.501146 9.105608 0.9911642 0.6044617 5 14.64 7.515865 8.498053 9.102729 0.9821873 0.6046762 6 16.11 7.441709 8.417347 9.020638 0.9756379 0.6032915 7 17.72 7.267367 8.255603 8.88203 0.9882355 0.6264277 8 19.49 7.105531 8.133438 8.783742 1.027907 0.6503038 9 21.44 7.025736 8.073084 8.733415 1.047348 0.6603308 10 23.58 6.970555 8.024835 8.691433 1.054279 0.6665983 11 25.94 6.88339 7.956075 8.63653 1.072685 0.6804547 12 28.53 6.819172 7.901899 8.59342 1.082727 0.6915207 13 31.38 6.815528 7.881151 8.569758 1.065623 0.6886077

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14 34.52 6.778287 7.84915 8.545932 1.070863 0.6967816 15 37.97 6.768456 7.825531 8.517666 1.057076 0.6921344 16 41.77 6.690573 7.758854 8.461597 1.068281 0.7027435 17 45.95 6.576372 7.672137 8.395837 1.095766 0.7236996 18 50.54 6.378003 7.54169 8.303526 1.163687 0.7618356 19 55.60 6.272883 7.465623 8.244529 1.192739 0.7789059 20 61.16 6.192893 7.405949 8.197833 1.213056 0.7918844 21 67.28 6.070224 7.315245 8.131417 1.245021 0.8161726 22 74.00 5.980441 7.250807 8.084737 1.270366 0.83393 23 81.40 6.003924 7.328994 8.150055 1.32507 0.8210607 24 89.54 5.761503 7.09622 7.970737 1.334717 0.8745165 25 98.50 5.668857 7.030812 7.924924 1.361955 0.8941116 26 108.35 5.626123 6.995907 7.896285 1.369784 0.9003778 27 119.18 5.520816 6.929633 7.853443 1.408817 0.92381 28 131.10 5.454289 6.885037 7.822189 1.430748 0.9371519 29 144.21 5.391116 6.846087 7.797658 1.454971 0.9515715 30 158.63 5.330243 6.807044 7.771194 1.476801 0.9641504 31 174.49 5.270195 6.777694 7.752686 1.507499 0.9749918 32 191.94 5.173338 6.724012 7.715868 1.550674 0.9918556 33 211.14 5.134089 6.704271 7.702201 1.570182 0.99793 34 232.25 5.115785 6.693449 7.693737 1.577663 1.000288

# Table b.tab Tue 13:37:45 25Jul2006

# row SMA INTENS INT_ERR PIX_VAR RMS ELLIP ELLIP_ERR PA# pixel degrees

1 10.00 852. 43.2 457. 323. 0.2000 INDEF 20.00 2 11.00 903. 60.9 678. 480. 0.2000 INDEF 20.00 # row PA_ERR X0 X0_ERR Y0 Y0_ERR GRAD GRAD_ERR GRAD_R_ERR# degrees pixel pixel pixel pixel

1 INDEF 485.00 INDEF 545.00 INDEF 0.04 INDEF INDEF 2 INDEF 485.00 INDEF 545.00 INDEF 0.032 INDEF INDEF

# row RSMA MAG MAG_LERR MAG_UERR TFLUX_E TFLUX_C TMAG_E# pixel**1/4

1 1.77828 7.33 0.0564 0.0536 202146. 254556. 13.3 2 1.82116 7.39 0.0759 0.0709 247010. 306532. 13.5

# row TMAG_C NPIX_E NPIX_C A3 A3_ERR B3 B3_ERR A4

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#

1 13.5 251 317 78.8 93.8 98.5 105. 334. 2 13.7 301 377 303. 343. 349. 369. 623.

# row A4_ERR B4 B4_ERR NDATA NFLAG NITER STOP A_BIG SAREA# pixel

1 272. 31.2 57.6 56 0 2 4 356. 2.0 2 548. 10.4 227. 62 0 1 4 137. 2.0

# row magb#

1 7.326419 2 7.388693

is> tprint b1.tab

# Table b1.tab Tue 13:54:28 25Jul2006

# row SMA magb# pixel

1 10.00 7.326419 2 11.00 7.388693 3 12.10 7.452424

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14Iraf Installation1FOR REDHAT FEDORA

Download these three files first.

Create iraf tree.(using root in / ) /iraf

/ \ (AS) /iraf /irafbin

/ \ (IB) bin.redhat noao.bin.redhat (NB)

Put the files in the respective as shown in above figure .gunzip it and untar it,by the command,withinthe respective folder.

Simply rm rf iraf/ irafbin/ x11iraf/ extern/echo 'making directroy structure'mkdir irafmkdir irafbinmkdir irafbin/bin.redhatmkdir irafbin/noao.bin.redhatmkdir externmkdir x11irafmkdir extern/stsdasmkdir extern/stsdas/bin.redhatmkdir extern/tablesmkdir extern/tables/bin.redhatmkdir extern/fitsutilecho 'Unpacking the file system' cd /iraf/iraftar zxf /iraf/redhat.package/as.pcix.gen.gzcd /iraf/irafbin/bin.redhattar zxf /iraf/redhat.package/ib.rhux.x86.gzcd /iraf/irafbin/noao.bin.redhattar zxf /iraf/redhat.package/nb.rhux.x86.gzcd /iraf/x11iraftar zxf /iraf/redhat.package/x11irafv1.3.1bin.redhat.tar.gzcd /iraf/extern/stsdas

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tar zxf /iraf/redhat.package/stsdas33.tar.gzcd /iraf/extern/stsdas/bin.redhattar zxf /iraf/redhat.package/stsdas33.bin.rh.tar.gzcd /iraf/extern/tablestar zxf /iraf/redhat.package/tables33.tar.gzcd /iraf/extern/tables/bin.redhattar zxf /iraf/redhat.package/tables33.bin.rh.tar.gzecho 'installing the x11' cd /iraf/x11iraf./installecho 'installing the iraf' cd /iraf/iraf/unix/hlib./installcd /irafecho 'please check the /iraf/iraf/unix/hlib/extern.pkg'

Of course then move the downloaded Xgterm.fedora &ds9 to the /usr/local/bin.

***********************************************************************Part3

[chrisphin@aries25 ~]$ mkiraf creating a new uparm directoryTerminal types: xgterm,xterm,gterm,vt640,vt100,etc.Enter terminal type: xgtermA new LOGIN.CL file has been created in the current directory.You may wish to review and edit this file to change the defaults.and then for externing the package of stsdas go to >cd /iraf/iraf/unix/hlib>vi extern.pkg

edit the earlier commands like shown below...# External (non coresystem) packages. To install a new package, add the

# two statements to define the package root directory and package task,# then add the package helpdb to the `helpdb' list.

reset noao = iraf$noao/task noao.pkg = noao$noao.cl

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reset tables = /iraf/extern/tables/task tables.pkg = tables$tables.cl

reset stsdas = /iraf/extern/stsdas/task stsdas.pkg = stsdas$stsdas.cl

reset helpdb = "lib$helpdb.mip\ ,noao$lib/helpdb.mip\ ,tables$lib/helpdb.mip\ ,stsdas$lib/helbdb.mip\ "

keep

That's it.

14.1How it's works [root@aries25 chrisphin]#mkdir iraf[root@aries25 chrisphin]#cd iraf

within this put this folder iraf.V2.12a.tgz

[root@aries25 iraf]# gunzip iraf.V2.12a.tgz[root@aries25 iraf]# lsiraf.V2.12a.tar[root@aries25 iraf]# tar xvpf iraf.V2.12a.tariraf.installredhat.package/redhat.package/as.pcix.gen.gzredhat.package/tables33.bin.rh.tar.gzredhat.package/ib.rhux.x86.gzredhat.package/x11irafv1.3.1bin.redhat.tar.gzredhat.package/xgterm.fedoraredhat.package/tables33.tar.gzredhat.package/stsdas33.bin.rh.tar.gzredhat.package/stsdas33.tar.gzredhat.package/nb.rhux.x86.gz[root@aries25 iraf]# ./iraf.installremoving the existing directory structure for iraf

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making directroy structureUnpacking the file systeminstalling the x11

X11IRAF V1.3 Installation =========================

Binary Installation:

The local commands directory is the place where the commands such as 'xgterm' and 'ximtool' will be installed. This should be a directory in a common search path such as /usr/local/bin.

Local commands directory (/usr/local/bin):

Installing new binaries in /usr/local/bin ...[ OK ]

Manual Page Installation:

Man pages are available for each of the X11IRAF tasks, some tasks will also provide online documentation. Manual pages may be installed either in the main system directory or in a local directory as long as that is accessible through a MANPATH environment variable.

Local man page directory (/usr/share/man/man1):[ OK ]

Application Default Resource Installation:

The appdefaults directory contains the default X resources for the XGterm task. This is not required for the program to work but provides for more readable menu entries, fonts, etc. The directory is normally part of the X11 tree but may be any directory specified in an XFILESEARCHPATH environment variable.

81


System appdefaults directory (/usr/lib/X11/appdefaults):...[ OK ]

Client Display Library (CDL) Installation:

The CDL is an interface for C/Fortran programs to display images to XImtool and compatible display servers. This library is not required in the runtime system for XImtool but can be useful for developing local applications needing a display capability. The local lib directory is the place where the CDL library file will be installed, the local include directory is where the needed nclude files for the library will be installed.

Would you like to install this library? (yes):Local lib directory (/usr/local/lib):

Installing CDL libraries in /usr/local/lib ...[ OK ]

Local include directory (/usr/local/include):

Installing include files in /usr/local/include ...[ OK ]

Installation complete.

installing the iraf

IRAF V2.12.1 System Installation ================================

Welcome to the IRAF installation script. This script will first prompt you for several needed path names. The system will be verified for proper structure before the actual install begins, all error must must be corrected before you will be allowed to continue. Recommend ations for fixing problems will be made but no corrective action will be taken directly. Once properly installed, you will be allowed to do some minimal configuration.

82


For each prompt: hit <CR> to accept the default value, 'q' to quit, or 'help' or '?' to print an explanation of the prompt.

============================================================================================= Query for System Settings ==============================================================================================

New iraf root directory (/iraf/iraf):Default root image storage directory (/iraf/imdirs):Local unix commands directory (/usr/local/bin):

============================================================================================= Verifying System Settings ==============================================================================================

Hostname = aries25.upso.ernet.i OS version = Linux 2.6.91.667smpArchitecture = redhat HSI arch = redhatNew iraf root = /iraf/iraf Old iraf root = /iraf/irafNew imdir = /iraf/imdirs Old imdir = /d0/imdirsLocal bin dir = /usr/local/bin

Checking definition of iraf root directory ... [ OK ]Checking iraf root and imdir directory ... [ OK ]Checking iraf directory write permissions ... [ OK ]Checking for iraf user account ... [ WARN ]

*** No 'iraf' user was found in the /etc/passwd file. The iraf *** user should be created before installing the system to ensure *** all files are owned by the iraf user, and the have the proper *** environment defined for installation and maintanence.

Checking file ownerships ... [ WARN ]

*** (root dir owned by 312, iraf files owned by 312)

83


*** The iraf tree should be owned by the iraf user so it can *** be updated and maintained properly. *** *** To fix this, login as root, set the iraf environment, and *** issue the commands: *** *** cd /iraf *** chown R iraf . # change dir owner *** cd $hbin # go to HSI bin dir *** chown 0 alloc.e # fix alloc.e ownership *** chmod 4755 alloc.e # fix permissions

Checking file permissions ... [ OK ]Checking proper iraf tree structure in /iraf ... Checking for 'iraf' subdir ... [ OK ] Checking for 'irafbin' subdir ... [ OK ] Checking for 'irafbin/bin.redhat' subdir ... [ OK ] Checking for 'irafbin/noao.bin.redhat' subdir ... [ OK ]Checking Core system binary directory ... [ OK ]Checking NOAO package binary directory ... [ OK ]Checking that local bin directory exists ... [ OK ]Checking for existing commands directory... [ OK ]

Proceed with installation? (yes):================================================================================================= Begin Installation =================================================================================================

Editing Paths Editing the iraf user .login/.cshrc paths ... [ OK ]Editing iraf/imdir paths into system files ... [ OK ]

Checking File Permissions Checking iraf file permissions ... [ OK ]Creating root imdir at /iraf/imdirs ... [ OK ]Reset /tmp sticky bit setting ... [ OK ]

84


Setting tape device permissions ... [ OK ]Checking alloc.e permissions ... [ OK ]

Creating File Links Checking for /iraf symlink ... [ OK ]Checking /usr/include directory ... [ OK ]Creating <iraf.h> symlink ... [ OK ]Creating iraf command links in local bin dir ... [ OK ]Marking system update time hlib$utime ... [ OK ]

Creating Graphics Device Files Creating /dev/imt1 fifo pipes for image display ... [ OK ]Creating /dev/imt fifo pipes link ... [ OK ]Checking /usr/local/lib directory ... [ OK ]Creating /usr/local/lib/imtoolrc link ... [ OK ]Checking if termcap file contains an XGterm entry ... [ OK ]Checking graphcap file for XGterm/imtool entries ... [ OK ]

============================================================================================= PostInstall Configuration =============================================================================================

The system should be fully functional at this point however somepostinstall configuration may be required to make use of all thefeatures such as networking or tape access. Additional software suchas external packages or display servers will need to be installedseparately. Some minimal configuration can be accomplished now butyou should consult the IRAF Site Manager's Guide for a more completediscussion of IRAF system management, configuration of printers, etc.

Proceed to postinstall configuration stage? (yes): IRAF Networking Config

IRAF Networking can be used to access a remote image, tape device,

85


display server, or other network service. It's configuration is nota requirement for normal IRAF operations and it can be updated at anytime by editing the IRAF dev$hosts file with new entries.

In this stage we will add an entry for the current platform to thehosts file. In a local network installation this script should be runon each system to add a networking entry as well as to install othersystem files needed by IRAF.

Configure IRAF Networking on this machine? (yes):Recommended dev$hosts file entry used for this machine:

aries25 aries25.upso.ern : aries25.upso.ernet.in!/iraf/iraf/bin.redhat/irafks.e

Proceed with this entry? (yes):

Creating backup of default dev$hosts file...Initializing dev$hosts file ...Host 'aries25.upso.ernet.in' has been added to the network configuration file...Checking that iraf networking is properly enabled ... [ OK ]

Tapecap Device File Config

By default IRAF will search for a dev$tapecap.<node> file (where<node> is the system name) when looking for a tape configuration file.Platforms such as PCIRAF and Sun/IRAF support multiple OS versionsand so the proper template file must be used. This configuration willallow you to setup a default tapecap for this system, it may be skippedif this machine has no tape drive attached.

Create a default tapecap file? (yes):Creating default file 'tapecap.aries25.upso.ern' from tapecap.linux...

In the event a dev$tapecap.<node> file is not found on thissystem IRAF will fallback to use just dev$tapecap. In cases wherethe node name changes, this installation is shared with another

86


machine or in a local network, or any case where a tapecap.<node>is not found, the dev$tapecap file will be the default tapecap usedfor all IRAF systems.

Do you wish to create a default dev$tapecap link? (yes):Tapecap symlink 'tapecap' exists and is ok.

Delete Unneeded HSI Binaries

The following bin directories in the iraf$unix directories werefound to be unused on this machine:

( 4768 Kb) /iraf/iraf/unix/bin.freebsd ( 2040 Kb) /iraf/iraf/unix/bin.linux ( 3540 Kb) /iraf/iraf/unix/bin.linuxppc ( 3460 Kb) /iraf/iraf/unix/bin.macosx ( 2480 Kb) /iraf/iraf/unix/bin.sunos ( 2432 Kb) /iraf/iraf/unix/bin.suse

The contents of these directories may be safely deleted to reclaimabout 18 Mb of disk space without affecting the IRAF runtime system.

Do you wish to delete these unused HSI binaries? (yes):Delete HSI binaries in bin.freebsd ... [ OK ]Delete HSI binaries in bin.linux ... [ OK ]Delete HSI binaries in bin.linuxppc ... [ OK ]Delete HSI binaries in bin.macosx ... [ OK ]Delete HSI binaries in bin.sunos ... [ OK ]Delete HSI binaries in bin.suse ... [ OK ]

Strip IRAF System Sources

Source code for all IRAF tasks and interfaces is included with thisinstallation, but is strictly only required if you plan to develop this

87


code. The sources may be deleted from the system without affecting theruntime environment (including help pages, compilation of external packages or local task development) allowing you to reclaim 5060Mb of diskspace for the system. Stripping sources is recommended for systems veryshort on space, leaving it on the system will allow IRAF site support tosend code fixes and compilation instructions as needed to fix problemswhich have no other workaround.

Do you wish to strip the system of sources? (no):============================================================================================= PostInstall Verification ==============================================================================================

Display Server Availability

Display Servers Found on This Machine:

( Date: 6 10:02 /usr/local/bin/ximtool ) /usr/local/bin/ximtool ( Date: 6 10:02 /usr/local/bin/ximtoolalt ) /usr/local/bin/ximtoolalt ( Date: 8 2004 /usr/local/bin/ds9 ) /usr/local/bin/ds9

Graphics Terminal Availability

Graphics Terminals Found on This Machine:

( Date: 6 10:02 /usr/local/bin/xgterm ) /usr/local/bin/xgterm ( Date: 14 2004 /usr/bin/xterm ) /usr/bin/xterm

========================================================================Congratulations! IRAF has been successfully installed on this system.

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========================================================================

To begin using the system simply log in as any user and from thedirectory you wish to use as your iraf login directory type:

% mkiraf # create a login.cl file % cl # start IRAF

The 'iraf' user is already configured with a login.cl file so a simple'cl' command is sufficient to start the system.

Additional information can be found at the IRAF web site:

http://iraf.noao.edu

Please contact site support with any questions or problems at

[email protected]

======================================================================================== Installation Completed With No Errors =======================================================================================

please check the /iraf/iraf/unix/hlib/extern.pkg Thanx chrisphin[root@aries25 iraf]#exit

[chrisphin@aries25 ~]$ mkiraf creating a new uparm directoryTerminal types: xgterm,xterm,gterm,vt640,vt100,etc.Enter terminal type: xgtermA new LOGIN.CL file has been created in the current directory.You may wish to review and edit this file to change the defaults.and then for externing the package of stsdas go to

89


>cd /iraf/iraf/unix/hlib>vi extern.pkg

edit the earlier commands like shown below...# External (non coresystem) packages. To install a new package, add the

# two statements to define the package root directory and package task,# then add the package helpdb to the `helpdb' list.

reset noao = iraf$noao/task noao.pkg = noao$noao.cl

reset tables = /iraf/extern/tables/task tables.pkg = tables$tables.cl

reset stsdas = /iraf/extern/stsdas/task stsdas.pkg = stsdas$stsdas.cl

reset helpdb = "lib$helpdb.mip\ ,noao$lib/helpdb.mip\ ,tables$lib/helpdb.mip\ ,stsdas$lib/helbdb.mip\ "

keep

That's it.

HAVE A FUN.

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IGeneral

For Aries 40 inch:

Readout Noise: 5.3 eGain : 10 e/ADUSaturation level:28000

For HCT: Readout noise is : 4.8 Gain is : 1.22Saturation level : 63000

CALCULATING AIRMASS THROUGH MIDAS:Midas 016> compute/airmass 13,23,35.2 36,07,59.5 ? 300 79,28,00 29,21,36 2006,5,03 17,20,00Julian date: 2.453859222222E+06Local mean sidereal time: 13 : 23 : 44.155Airmass: 1.00707E+00Midas 017>

Midas 016> compute/airmass RA DEC S.T EXPOTIME LONG LATI YYYY/M/DD UT

If dont know the ST just type ? in that place

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II.Airmass Calculation Program

# Define variables.

# observatory = "IAO"

long = 281:02.15lat = 32:46.77

ut = sexstr ((@'tm_start'+0.1) / 3600.)# obd = sexstr(@'dateobs')a# This is for 2k2nov15 (yy:mm:dd) ep = epoch ('20060312',ut) jd = julday ('20060312',ut) st = mst ('20060312',ut, long) rap = ra_precess (ra, dec, ep, 2000) dap = dec_precess (ra, dec, ep, 2000)

HA = rap st airmass = airmass (rap, dap, st, lat) # print(obd) print(ut)

print(ep)print(jd)print(st)print(airmass)

# airmass = eairmass (ra, dec, mst, itime, obsdb (observat, "latitude"))

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III.FEAR FeAr Line List 3000A10,000A by D. Willmarth# units Angstroms

3443.8762 FeI3722.5625 FeI3859.9114 FeI4033.8093 ArII4158.5905 ArI4198.3036 FeI4348.0640 ArII4427.3039 FeI4545.0519 ArII4657.9012 ArII4764.8646 ArII4879.8635 ArII4965.0795 ArII5167.4873 FeI5227.1697 FeI5269.5366 FeI5328.0376 FeI5371.4892 FeI5606.7330 ArI5912.0853 ArI6032.1274 ArI6114.9234 ArII6416.3071 ArI6677.2817 ArI6752.8335 ArI6871.2891 ArI6965.4307 ArI7067.2181 ArI7272.9359 ArI7383.9805 ArI7635.1060 ArI

93


IV.Spectrum Extinction file for IAO (spec_ext.dat)

3000. 0.709266663 3050. 0.666614115 3100. 0.62731874 3150. 0.591068327 3200. 0.557584167 3250. 0.526616693 3300. 0.497942328 3350. 0.471360266 3400. 0.446689993 3450. 0.423768848 3500. 0.402450085 3550. 0.382601142 3600. 0.364102066 3650. 0.346844196 3700. 0.330728948 3750. 0.315666676 3800. 0.301575929 3850. 0.288382441 3900. 0.27601853 3950. 0.264422387 4000. 0.253537506 4050. 0.24331215 4100. 0.233698964 4150. 0.224654481 4200. 0.21613881 4250. 0.208115265 4300. 0.200550109 4350. 0.193412289 4400. 0.186673149 4450. 0.180306271 4500. 0.174287245 4550. 0.168593511 4600. 0.163204208 4650. 0.158099994 4700. 0.153262973 4750. 0.14867653 4800. 0.144325256 4850. 0.140194833 4900. 0.136271924 4950. 0.13254416 5000. 0.129000008 5050. 0.125628695 5100. 0.122420244 5150. 0.119365282 5200. 0.116455086 5250. 0.113681495 5300. 0.111036889 5350. 0.108514145 5400. 0.106106579 5450. 0.103807941

94


5500. 0.101612359 5550. 0.0995143577 5600. 0.0975087583 5650. 0.0955907404 5700. 0.0937557369 5750. 0.0919994786 5800. 0.0903179497 5850. 0.0887073651 5900. 0.0871641561 5950. 0.0856849775 6000. 0.0842666626 6050. 0.0829062387 6100. 0.0816008821 6150. 0.0803479403 6200. 0.0791449174 6250. 0.0779894367 6300. 0.0768792704 6350. 0.0758122951 6400. 0.0747865066 6450. 0.0738000199 6500. 0.0728510395 6550. 0.0719378665 6600. 0.0710588917 6650. 0.0702125877 6700. 0.0693975165 6750. 0.0686122924 6800. 0.0678556263 6850. 0.0671262667 6900. 0.0664230511 6950. 0.0657448545 7000. 0.0650906265 7050. 0.0644593537 7100. 0.0638500676 7150. 0.0632618666 7200. 0.062693879 7250. 0.0621452704 7300. 0.0616152622 7350. 0.0611030944 7400. 0.0606080554 7450. 0.0601294637 7500. 0.0596666671 7550. 0.05921904 7600. 0.0587859936 7650. 0.0583669618 7700. 0.0579614006 7750. 0.057568796 7800. 0.0571886562 7850. 0.0568205081 7900. 0.0564638972 7950. 0.0561183989 8000. 0.0557835922 8050. 0.0554590896

95


8100. 0.0551445074 8150. 0.0548394881 8200. 0.0545436852 8250. 0.0542567633 8300. 0.0539784022 8350. 0.0537083037 8400. 0.0534461737 8450. 0.0531917289 8500. 0.0529447012 8550. 0.0527048372 8600. 0.0524718799 8650. 0.052245602 8700. 0.0520257652 8750. 0.0518121608 8800. 0.051604569 8850. 0.0514027961 8900. 0.0512066409 8950. 0.0510159172 9000. 0.0508304499 9050. 0.0506500639 9100. 0.0504745916 9150. 0.0503038764 9200. 0.050137762 9250. 0.0499760993 9300. 0.0498187467 9350. 0.0496655703 9400. 0.0495164357 9450. 0.0493712127 9500. 0.0492297821 9550. 0.0490920246 9600. 0.0489578284 9650. 0.0488270782 9700. 0.048699677 9750. 0.0485755131 9800. 0.0484544933 9850. 0.0483365245 9900. 0.0482215099 9950. 0.0481093638 10000. 0.0480000004 10050. 0.0478933342 10100. 0.0477892905 10150. 0.047687795 10200. 0.0475887656 10250. 0.0474921316 10300. 0.0473978296 10350. 0.0473057851 10400. 0.0472159423 10450. 0.0471282303

96


V.Extinction Coefficients for ARIESThe extinction coeff. measured for Dec2, 2005 is given below for each filter.

U 0.458727+/0.010090B 0.245316+/ 0.010248V 0.134039+/0.004601R 0.091876+/0.002154I 0.050587+/0.002275

The transformation coeff. for the same night is given below. The first colum is the equation used, second column is the slope, then error in slope, then intercept, error in intercept.

slope error intercept error BVbv 0.994553 0.01317 0.346141 0.01704 VvBV 0.0179182086 0.0177878 3.2054812 0.01676718RIri 1.04770505 0.0323265 0.531954765 0.007405 UBub 0.86043411 0.0232752 1.61161196 0.05531368 VIvi 0.99450880 0.023112 0.5001866 0.016288 VvVI 0.018754551 0.0165158 3.2085557 0.01765941 VRvr 0.947630703 0.030370 0.01078140 0.017623 VRvr 0.934882 0.02597 0.0220804 0.01542 VvVR 0.0364902467 0.0308615 3.2083962 0.016983876 UuUB 0.1290 0.03 5.4014 0.02

The extinction correction u can give like this.u0=uKu * Xb0=bKb * Xv0=vKv * Xr0=rKr * Xi0=iKi *X

where, ubvri are the observed magnitudes(without any correction)u0, b0,v0,r0, i0 are th extinction corrected using the above relationKu,Kb,Kv,Kr,Ki are the extinctions coeffs. which is given above for

97


each filters. X is the respective airmasses.

then the eqns. for giving transformation coeffs. is given below.

(UB) = a1 * (u0b0)+a2(BV) = b1 * (b0v0)+b2(VI) = c1 * (v0i0)+c2(VR) = d1 * (v0r0)+d2(RI) = e1 * (r0i0)+e2

Vv0 = f1 * (BV)+f2Vv0 = g1 * (VR)+g2......This way u can make any combination of eqns. here a1,a2,b1,b2,c1,c2.... etc are the std coeffs. which is given above.u can directly use those coefficients. and UBVRI are the std magnitude fromthe Landolt.

After rearranging the last two eqns, u can get the final std V mag. then from V std mag,u can get std mag for any other filters.

Location, Nainital is situated at 29 degree 24' north latitude and 79 degree 28' east longitude. Altitude,1938 Meters or 6360 ft, above sea level.

98


VI.Site Characteristics of HCT

Latitude 32d46m46s N

Longitude78d57m51s E

Altitude4500 meters above msl

SeismicityLow

Wind SpeedMedian 2.2 m/s (8 kmph) at night

Wind DirectionPrevailing southsoutheasterly

Low ambient temperature and very lowhumidity

Annual precipitation of rain & snow< 7 cm

Precipitable water vapour< 2 mm between October and April

Number of spectroscopic nights~ 260 per year

Number of photometric nights~ 190 per year

Median seeing< 1 arcsec

Uniform distribution of useful nights roundthe year

Longitudinal advantage(79d E) Canary Islands (20d W); EasternAustralia(157d E)

Good accessibility round the yer

99


VII.Extinction and Sky Brightness for HCT

Mean Extinction Values (2000 December 2003 January)

U0.353 +/ 0.037

B0.209 +/ 0.029

V0.121 +/ 0.032

R0.0823 +/ 0.037

I0.0497 +/ 0.027

Mean night sky brightness (1995 & 2002)

U23.64 +/ 0.57

B22.94 +/ 0.50

V21.52 +/ 0.21

R20.20 +/ 0.35

I18.60 +/ 0.21

100


VIII .Halpha filter response curve for HCT

101


IX.FeAr wavelength identification1

102


X.FeAr wavelength identification2

103


XI.FeNe wavelength identification

104


XII.Standard calibration data for extinction from IRAF

The onedstds$ directory contains standard calibration data for extinction andsensitivity calibration as used in the ONEDSPEC, TWODSPEC, and the variousIMRED packages.

EXTINCTION TABLES (eg extinction = onedstds$kpnoextinct.dat)

ctioextinct.dat CTIO extinction table for ONEDSPEC (in Angstroms) The CTIO extinction curve distributed with IRAF comes from the work of Stone & Baldwin (1983 MN 204, 347) and Baldwin & Stone (1984 MN 206, 241). The first of these papers lists the points from 32008370A while the second extended the flux calibration from 6056 to 10870A but the derived extinction curve was not given in the paper. The IRAF table follows SB83 out to 6436, the redder points presumably come from BS84 with averages used in the overlap region.

More recent CTIO extinction curves are shown as Figures in Hamuy et al (92, PASP 104, 533 ; 94 PASP 106, 566).

Steve Heathcote, Mon, 19 Jul 1999

kpnoextinct.dat KPNO extinction table for ONEDSPEC (in Angstroms)

MISCELLANEOUS

ctio Directory containing CTIO decker comb positions and neutral density filter curves (used with NDPREP).

FLUX STANDARD DIRECTORIES (eg caldir = onedstds$iidscal/)

blackbody Directory for using blackbody flux distributions in various magnitude bands.

bstdscal Directory of the brighter KPNO IRS standards (i.e. those with HR numbers) at 29 bandpasses, data from various sources transformed to the Hayes and Latham system,

105


unpublished. ctiocal Directory containing fluxes for the southern tertiary standards as published by Baldwin & Stone, 1984, MNRAS, 206, 241 and Stone and Baldwin, 1983, MNRAS, 204, 347. ctionewcal Directory containing fluxes at 50A steps in the blue range 33007550A for the tertiary standards of Baldwin and Stone derived from the revised calibration of Hamuy et al., 1992, PASP, 104, 533. This directory also contains the fluxes of the tertiaries in the red (605010000A) at 50A steps as will be published in PASP (Hamuy et al 1994). The combined fluxes are obtained by gray shifting the blue fluxes to match the red fluxes in the overlap region of 6500A7500A and averaging the red and blue fluxes in the overlap. The separate red and blue fluxes may be selected by following the star name with "red" or "blue"; i.e. CD 32 blue. iidscal Directory of the KPNO IIDS standards at 29 bandpasses, data from various sources transformed to the Hayes and Latham system, unpublished. irscal Directory of the KPNO IRS standards at 78 bandpasses, data from various sources transformed to the Hayes and Latham system, unpublished (note that in this directory the brighter standards have no values the `bstdscal' directory must be used for these standards at this time). oke1990 Directory of spectrophotometric standards observed for use with the HST, Table VII, Oke 1990, AJ, 99. 1621 (no correction was applied). An arbitrary 1A bandpass is specified for these smoothed and interpolated flux "points". Users may copy and modify these files for other bandpasses. redcal Directory of standard stars with flux data beyond 8370A. These stars are from the IRS or the IIDS directory but have data extending as far out into the red as the literature permits. Data from various sources. spechayescal The KPNO spectrophotometric standards at the Hayes flux points, Table IV, Spectrophotometric Standards, Massey et al., 1988, ApJ 328, p. 315. spec16cal Directory containing fluxes at 16A steps in the blue range 33007550A for the secondary standards, published in Hamuy et al., 1992, PASP, 104, 533. This directory

106


also contains the fluxes of the secondaries in the red (602010300A) at 16A steps as will be published in PASP (Hamuy et al 1994). The combined fluxes are obtained by gray shifting the blue fluxes to match the red fluxes in the overlap region of 6500A7500A and averaging the blue and red fluxes in the overlap. The separate red and blue fluxes may be selected by following the star name with "red" or "blue"; i.e. HR 1544 blue. spec50cal The KPNO spectrophotometric standards at 50 A intervals. The data are from (1) Table V, Spectrophotometric Standards, Massey et al., 1988, ApJ 328, p. 315 and (2) Table 3, The Kitt Peak Spectrophotometric Standards: Extension to 1 micron, Massey and Gronwall, 1990, ApJ 358, p. 344.

STANDARD STAR MENUS

Blackbody calibrations in onedstds$blackbody/

U B V R I J H K L Lprime M

Magnitude conversions are available between V, J, H, K, L, Lprime, and Mbut for U, B, R, and I the star magnitudes must be in the same bandpass.Standard stars in onedstds$bstdscal/

hr718 hr3454 hr3982 hr4468 hr4534hr5191 hr5511 hr7001 hr7596 hr7950hr8634 hr9087 hd15318 hd74280 hd100889hd188350 hd198001 hd214923 hd224926

Standard stars in onedstds$ctiocal/

bd25 eg139 feige56 l2415 l93080bd73632 eg149 feige98 l2511 l97030bd8 eg158 g16350 l3218 lds235cd32 eg248 g2631 l3864 lds749eg11 eg274 g9937 l4364 ltt4099

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eg21 f15 h600 l4816 ltt8702eg26 f25 hz2 l6248 ross627eg31 f56 hz4 l7379 w1346eg54 f98 hz15 l7987 w485aeg63 f110 kopf27 l8702 wolf1346eg76 feige110 l377 l9239 wolf485aeg79 feige15 l1020 l9491eg99 feige25 l1788 l74546

Standard stars in onedstds$ctionewcal/:

Combined red and blue 3300A10000A:

cd32 f56 l2415 l4364 l7987 eg21 h600 l3218 l4816 l9239 eg274 l1020 l377 l6248 l9491 f110 l1788 l3864 l7379 l745

Blue 3300A7550A:

cd32blue f56blue l2415blue l4364blue l7987blue eg21blue h600blue l3218blue l4816blue l9239blue eg274blue l1020blue l377blue l6248blue l9491blue f110blue l1788blue l3864blue l7379blue

Red 6050A10000A:

cd32red f56red l2415red l4364red l7987red eg21red h600red l3218red l4816red l9239red eg274red l1020red l377red l6248red l9491red f110red l1788red l3864red l7379red l745red

Standard stars in onedstds$iidscal/

40erib eg50 eg149 g16350 hz4 lds235bamcvn eg54 eg158 g191b2b hz7 lds749bbd253941 eg63 eg162 g2610 hz14 lft1655bd284211 eg67 eg182 g2631 hz15 lp414101

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bd332642 eg71 eg184 g4718 hz29 ltt13002bd404032 eg76 eg193 g88 hz43 ltt16294bd73632 eg77 eg247 g9937 hz44 ltt4099bd7781 eg79 eg248 gd128 kopff27 ltt8702bd82015 eg91 feige15 gd140 l13633 ross627eg11 eg98 feige24 gd190 l140349 ross640eg20 eg99 feige25 gh7112 l14094 sa29130eg26 eg102 feige34 grw705824 l151234b sao131065eg28 eg119 feige56 grw708247 l74546a ton573eg29 eg129 feige92 grw738031 l8702 wolf1346eg31 eg139 feige98 he3 l93080 wolf485aeg33 eg144 feige110 hiltner102 l97030 eg39 eg145 g12627 hiltner600 lb1240 eg42 eg148 g14563 hz2 lb227

Standard stars in onedstds$irscal/

bd082015 eg50 feige34 hd117880 hd60778 hr7001bd174708 eg71 feige56 hd161817 hd74721 hz44bd253941 eg139 feige92 hd17520 hd84937 kopff27bd262606 eg158 feige98 hd192281 hd86986 wolf1346bd284211 eg247 feige110 hd19445 he3 bd332642 feige15 g191b2b hd217086 hiltner102 bd404032 feige25 hd109995 hd2857 hiltner600

Standard stars in onedstds$oke1990/

bd284211 feige110 feige67 g191b2b g249 gd248 ltt9491 eg71bd75325 feige34 g13831 g19374 gd108 hz21 eg158 eg247

Standard stars in onedstds$redcal/

40erib eg63 eg139 eg248 gd140 hz44 ltt16294amcvn eg67 eg144 feige24 gd190 l13633 ltt4099bd7781 eg76 eg145 g12627 grw705824 l14094 ltt8702bd73632 eg79 eg148 g14563 grw708247 l151234b ross627bd174708 eg91 eg149 g16350 grw738031 l74546a ross640

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bd262606 eg98 eg162 g191b2b hd19445 l93080 sa29130eg20 eg99 eg182 g2610 hd84937 l97030 sao131065eg33 eg102 eg184 g2631 he3 lds235b wolf1346eg50 eg119 eg193 g4718 hz29 lds749b wolf485aeg54 eg129 eg247 g9937 hz43 lft1655

Standard stars in onedstds$spec16cal/:

Combined red and blue 3300A10300A:

hd15318 hd74280 hd114330 hd188350 hd214923hd30739 hd100889 hd129956 hd198001 hd224926hr1544 hr4468 hr5501 hr7596 hr8634 hr3454 hr4963 hr718 hr7950 hr9087

Blue 3300A7550A:

hd15318blue hd74280blue hd114330blue hd188350blue hd214923bluehd30739blue hd100889blue hd129956blue hd198001blue hd224926bluehr1544blue hr4468blue hr5501blue hr7596blue hr8634blue hr3454blue hr4963blue hr718blue hr7950blue hr9087blue

Red 6020A10300A:

hd15318red hd74280red hd114330red hd188350red hd214923redhd30739red hd100889red hd129956red hd198001red hd224926redhr1544red hr4468red hr5501red hr7596red hr8634red hr3454red hr4963red hr718red hr7950red hr9087red

Standard stars in onedstds$spec50cal/ (3200A 8100 A)

bd284211 eg247 feige34 hd192281 pg0205134 pg0934554 wolf1346cygob2no9 eg42 feige66 hd217086 pg0216032 pg0939262 eg139 eg71 feige67 hilt600 pg0310149 pg1121145 eg158 eg81 g191b2b hz14 pg0823546 pg1545035 eg20 feige110 gd140 hz44 pg0846249 pg1708602

Standard stars in onedstds$spec50cal/ (3200A 10200A)

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bd284211 eg247 feige34 g191b2b hz44 eg139 eg71 feige66 gd140 pg0823546 eg158 feige110 feige67 hilt600 wolf1346

Standard stars in onedstds$spechayescal/

bd284211 eg139 feige67 hd217086 pg0216032 pg0939262cygob2no9 eg158 feige110 hiltner600 pg0310149 pg1121145eg42 eg247 g191b2b hz14 pg0823546 pg1545035eg71 feige34 gd140 hz44 pg0846249 pg1708602eg81 feige66 hd192281 pg0205134 pg0934554 wolf1346

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Documents

Iraf-data Reduction Guide Chris